224th aas - american astronomical society · 224th aas boston, ma – june, 2014 meeting abstracts...

224th AASBoston, MA – June, 2014

Meeting Abstracts

Session Table of Contents100 – Welcome Address by AAS President David Helfand101 – Kavli Foundation Lecture, David Spergel: New Probes of DarkEnergy119 – LAD Posters Monday120 – Extrasolar Planet Posters121 – Pulsars, Neutron Stars, and Supernovae Posters122 – Instrumentation Posters123 – SPD Posters 1102 – Extrasolar Planets: Characterization and Theory103 – Solar Magnetism I104 – Solar Energetic Events I105 – Topics in Astrostatistics106 – Bridging Laboratory & Astrophysics: Atoms107 – Astronomy Research and Development Using Picosatellites108 – Fred Adams: Effects of Clusters on Planetary Systems andPossible Constraints on the Birth Environment of the Solar System110 – Long Time Domain Astronomy111 – Solar Energetic Events II112 – Solar Magnetism II113 – Extrasolar Planets: Detection114 – Bridging Laboratory & Astrophysics: Molecules115 – Cosmology, CMB, and Dark Matter116 – Jacqueline van Gorkom: Gas and Galaxy Evolution: from Voids toClusters117 – George Ellery Hale Prize, Tom Duvall: Waves Excited by Noise:Applications to Helioseismology and Beyond118 – Jonathan Grindlay: Time Domain Astronomy with the HarvardPlates: from Cepheids to DASCH200 – Sara Seager: Mapping the Nearest Stars for Exotic HabitableWorldsLAD Posters Tuesday218 – SPD Posters 2219 – Variable Stars, Binaries, and Compact Objects Posters220 – Molecular Clouds and Dust Posters221 – AGN, QSO, Blazars Posters222 – Evolution of Galaxies Posters223 – Young Stellar Objects, Star Formation, and Star Clusters Posters201 – On the Shoulders of Giants: Planets Beyond the Reach of KeplerI: What We Know Today and What We Would Like to Learn202 – Solar Surface and Interior I203 – History of Solar Physics204 – Black Holes, Pulsars, and Neutron Stars205 – Bridging Laboratory & Astrophysics: Dust & Ices206 – Evolution of Galaxies207 – Arne Henden: Citizen Science in the Age of Surveys210 – On the Shoulders of Giants: Planets Beyond the Reach of KeplerII: Demographics211 – Solar Surface and Interior II212 – CME I213 – The Galactic Center and Nearby Galaxies214 – Bridging Laboratory and Astrophysics: Planetary215 – Star Formation and Interstellar Medium216 – Karen Harvey Prize, Alexis Rouillard: Probing the Origin of SlowSolar Wind, Coronal Mass Ejections and Solar Energetic Particles byCombining Solar and Heliospheric Imagery with In-situ Measurements217 – Margaret Meixner: The Life Cycle of Dust in the MagellanicClouds: Insights from Spitzer and Herschel

300 – Rosanne DiStefano: New Opportunities in GravitationalMicrolensing and MesolensingLAD Posters Wednesday318 – Structure of the Early Universe Posters319 – Surveys and Large Programs Posters320 – Education and History Posters321 – The Sun and The Solar System Posters322 – Stars and Stellar Populations Posters323 – SPD Posters 3301 – On the Shoulders of Giants: Planets Beyond the Reach of KeplerIII: Ground-based Imaging and Spectroscopy302 – Chromosphere and Transition Region I303 – CME II304 – Observation and Theory for Multiverse305 – Bridging Laboratory & Astrophysics: Plasmas306 – Education and History307 – Sebastian Heinz: Jets On All Scales: A Phenomenological View ofCollimated Outflows and Their Importance for Cosmic Structure311 – On the Shoulders of Giants: Planets Beyond the Reach of KeplerIV: The Near Future312 – Corona I313 – Chromosphere and Transition Region (IRIS)314 – Star Clusters, Binaries, Multiples, and Planetary Companions315 – Bridging Laboratory & Astrophysics: Nuclear and Particles316 – Education and Public Outreach317 – Neal Evans: Star Formation in the Gould Belt: Star FormationRates, Evolutionary Timescales, and Implications for Star FormationTheories400 – Newton Lacy Pierce Prize Lecture, Nadia Zakamska: Quasars andTheir Effect on Galaxy FormationLAD Posters Thursday413 – LAD Late Posters414 – SPD Late Posters415 – Education and Public Outreach Posters416 – Extrasolar Planets Posters417 – Galaxies Near and Far Posters418 – Instrumentation Posters419 – Molecular Clouds, the ISM and YSOs Posters420 – Stars, Stellar Evolution and So On Posters421 – Stars: Variable and Explosive Posters422 – The Sun and The Solar System Posters423 – Topics in Cosmology Posters401 – Gamma-ray Constraints on the EBL and the IGMF I402 – Solar Wind and Heliospheric Connections403 – SPD/LAD Joint Session: Bridging Laboratory and Solar PlasmaStudies I404 – Stellar Atmospheres and Outflows405 – Instrumentation, Surveys, and Data406 – Steve Kawaler: The Kepler Mission's "Other" Legacy: The Comingof Age of Space-based Asteroseismology407 – Gamma-ray Constraints on the EBL and the IGMF II408 – Corona II409 – SPD/LAD Joint Session: Bridging Laboratory and Solar PlasmaStudies II410 – AGN, QSO, Blazars411 – Relativistic Astrophysics, Gravitational Lenses & Waves412 – Supernovae and White Dwarfs

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100 – Welcome Address by AAS President David HelfandPlenary Session – America Ballroom North/Central – 02 Jun 2014 08:00 AM to 08:30 AM

101 – Kavli Foundation Lecture, David Spergel: New Probes of Dark EnergyPlenary Session – America Ballroom North/Central – 02 Jun 2014 08:30 AM to 09:20 AMChair(s):David Helfand (Quest University Canada)

101.01 – New Probes of Dark EnergyDark energy seems to dominate today's universe. The talkwill begin by reviewing the astronomical evidence forcosmic acceleration. This cosmic acceleration implies eitherthat the dark energy is the primary component of our

universe or that general relativity is not valid oncosmological scales. The talk will focus on new probes ofdark energy with a focus on measurements by the WFIRSTmission and observations of the cosmic microwavebackground.Author(s): David Spergel (Princeton University)

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119 – LAD Posters MondayPoster Session – Essex Ballroom and America Foyer – 02 Jun 2014 09:00 AM to 06:30 PM

119.01 – Transition Probabilities andElectron Impact Excitation CollisionStrengths for Fe VIIExtensive calculations have been performed for electronimpact excitation collision strengths and oscillatorstrengths for the Fe VII extreme ultraviolet lines ofastrophysical importance. The collision strengths forfine-structure transitions are calculated in the B-splineBreit-Pauli R-matrix approach. The target wave\-functionshave been calculated in the multi\-configurationHartree-Fock method with term-dependent non-orthogonalorbitals. The close-coupling expansion includes 189fine-structure levels of Fe VII belonging to terms of theground $3p^63d^2$ and excited $3p^53d^3$,$3p^63d4l$, $3p^53d5s$, and $3p^63d5p$configurations. The effective collision strengths aredetermined from the electron excitation collision strengthsby integration over a Maxwellian distribution of electronvelocities. The excitation rates are calculated forfine-structure transitions at electron temperatures from10$^4$ to 10$^7$ K suitable for use in astrophysicalplasma modeling. Our results normally agree with theprevious R-matrix frame-transformation calculations.However, there are important differences for sometransitions with the previous calculations. The correctionsto the previous results are mainly due to more extensiveexpansions for the Fe VII target states. We were able togenerate more accurate target states than those used inthe previous collision calculations. In comparison withprevious calculations, we included all $3p^43d^3nl$correlation configurations which were found very importantfor accurate representation of the $3dnl$ states. We alsofound that correlation configuration with $3p-4f$ promotionare equally important and may considerably change thetarget CI expansions. This work was supported by NASAunder grant NNX11AB62G from the Solar and Heliophysicsprogram.Author(s): Swaraj Tayal (Clark Atlanta University), Oleg Zatsarinny(Drake University)

119.02 – Comprehensive Analyses of theSpectra of Iron-group ElementsFor many decades, the Atomic Spectroscopy Group at NISThas measured atomic data of vital use to astronomy andother fields using high resolution spectrometers that arefound in few other places in the world. These now includethe 2-m Fourier transform (FT) spectrometer covering theregion 285 nm to 5500 nm, the FT700 vacuum ultraviolet(VUV) FT spectrometer covering the region 143 nm to 900nm, and a 10.7-m normal incidence spectrograph (NIVS)covering 30 nm to 500 nm. Recent work focused on themeasurement and analysis of wavelengths and energylevels of iron-group elements to provide extensive data forthe analysis of astrophysical spectra. Our comprehensivelinelist for Fe II from 90 nm to 5500 nm contains over 13600 lines with order of magnitude improvements in thewavelengths compared to previous work [Nave &Johansson, ApJSS 204, 1(2013)]. The spectra were observedin high-current continuous and pulsed hollow cathode (HCL)discharges using FT spectrometers and our NIVSspectrograph. A similar analysis of Cr II contains over 5300lines and extends the knowledge of this spectrum to thepreviously unobserved region between 731 nm at 5500 nm[Sansonetti, Nave, Reader & Kerber, ApJSS 202, 15 (2012);Sansonetti & Nave, ApJSS (in prep.)]. Our analysis of the CoIII spectrum contains 750 lines observed in Penningdischarge lamps and an additional 900 lines compiled fromprevious work, including Ritz wavelengths, optimizedenergy levels, and calculated log(gf) values [Smillie,Pickering, Nave & Smith, ApJSS (in prep.)]. NIST and ICL arecurrently collaborating to complete the measurement andanalysis of wavelengths, energy levels, and hyperfinestructure parameters for all singly-ionized iron-groupelements of astrophysical interest, covering the wavelengthrange 80 nm to 5500 nm. This project uses archival datafrom FT spectrometers at NIST, ICL and Kitt Peak NationalObservatory, with additional spectra of HCL and Penningdischarge sources taken using our FT and NIVSspectrometers. Current work includes the spectra of Mn I,Mn II, Ni II, Sc II, and Co III. This work was partiallysupported by NASA, the STFC and PPARC (UK), the RoyalSociety of the UK, and the Leverhulme Trust.Author(s): Gillian Nave (NIST), Craig Sansonetti (NIST), Juliet Pickering(Imperial College London), Florence Liggins (Imperial College London)

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119.03 – AtomPy: an open atomic-datacuration environmentWe present a cloud-computing environment for atomic datacuration, networking among atomic data providers andusers, teaching-and-learning, and interfacing with spectralmodeling software. The system is based on Google-DriveSheets, Pandas (Python Data Analysis Library) DataFrames,and IPython Notebooks for open community-driven curationof atomic data for scientific and technological applications.The atomic model for each ionic species is contained in amulti-sheet Google-Drive workbook, where the atomicparameters from all known public sources are progressivelystored. Metadata (provenance, community discussion, etc.)accompanying every entry in the database are storedthrough Notebooks. Education tools on the physics ofatomic processes as well as their relevance to plasma andspectral modeling are based on IPython Notebooks thatintegrate written material, images, videos, and activecomputer-tool workflows. Data processing workflows andcollaborative software developments are encouraged andmanaged through the GitHub social network. Relevantissues this platform intends to address are: (i) data qualityby allowing open access to both data producers and usersin order to attain completeness, accuracy, consistency,provenance and currentness; (ii) comparisons of differentdatasets to facilitate accuracy assessment; (iii)downloading to local data structures (i.e. PandasDataFrames) for further manipulation and analysis byprospective users; and (iv) data preservation by avoidingthe discard of outdated sets.Author(s): Manuel Bautista (Western Michigan University), ClaudioMendoza (Western Michigan University), Josiah Boswell (Western MichiganUniversity), Chukwuemeka Ajoku (Western Michigan University)

119.04 – Revised Term Values for the A–X

(v?=0-9, v?=0) Bands in 13C16O fromHigh-resolution Fourier Transform SpectraHigh-resolution spectra of the A 1? – X 1?+ band system of13C16O are presented. They were acquired with thevacuum ultraviolet (VUV) Fourier transform spectrometerinstalled on the DESIRS beamline at the SOLEILsynchrotron. We obtained revised term values that extendto higher J? values than previous VUV measurements formost v? levels and lower J? values for v?=0. Such data areneeded to model the A – X bands in spectra of astronomicalobjects, including diffuse molecular clouds, circumstellardisks around newly formed stars, and comets. Previouslyobserved perturbations of the rotational levels areconfirmed, but are seen now in greater detail, and evidenceis presented for new perturbations. The uncertainty in theline positions and term values of most CO transitions is on

average within 0.01 cm-1.Author(s): Steven Federman (Univ. of Toledo), Lisseth Gavilan (Obs.de Paris), Jean Louis Lemaire (Obs. de Paris), Michele Eidelsberg (Obs. deParis), Glenn Stark (Wellesley College), Alan Heays (Leiden Obs.),Jean-Hugues Fillion (UPMC Univ. Paris VI), James Lyons (ASU), Nelson deOliveira (Synchrotron SOLEIL)

119.05 – Merged beam studies forastrobiologyThe chain of chemical reactions leading towards life isthought to begin in molecular clouds when atomic carbonand oxygen are fixed into molecules. Reactions of neutral

atomic C with H3+ is one of the first steps in the gas phase

chemistry leading to the formation of complex organicmolecules within such clouds. Water, believed to be vital forlife, can form via a chain of gas-phase astrochemicalreactions that begin with neutral atomic O reacting with

H3+. Uncertainties in the thermal rate coefficient for these

reactions hinder our ability to understand the first links inthe chemical chain leading towards life. Theory andexperiment have yet to converge in either the magnitudeor temperature dependence. Theory provides little insightas fully quantum mechanical calculations for reactionsinvolving four or more atoms are too complex for currentcapabilities. On the other hand, measurements of crosssections and rate coefficients for reactions of atoms withmolecular ions are extremely challenging. This is due to thedifficulty in producing sufficiently intense and wellcharacterized beams of neutral atoms. We have developeda novel merged beam apparatus to study reactions ofneutral atoms with molecular ions at the low collisionenergies relevant for molecular cloud studies.Photodetachment of atomic anion beams, with an 808-nm(1.53-eV) laser beam, is used to produce beams of neutralC and O, each in their ground term as occurs in molecularclouds. The neutral beam is then merged with a velocity

matched, co-propagating H3+ beam, in order to study

reactions of C and O on H3+. The merged beams method

allows us to use fast beams (keV in the lab frame), whichare easy to handle and monitor, while being able to achieverelative collision energies down to ?10 meV. Using themeasured merged beams rate coefficient, we are able toextract cross sections which we can then convolve with aMaxwellian energy spread to generate a thermal ratecoefficient for molecular cloud temperatures. Here we

report recent results for reactions of C and O on H3+. This

work was funded in part by the NSF.Author(s): Nathalie De Ruette (Columbia University), Kenneth Miller(Columbia University), Aodh O'Connor (Columbia University), Julia Stuetzel(Columbia University), Xavier Urbain (Université catholique de Louvain),Daniel Savin (Columbia University)

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119.06 – Analysis Of The Returned SamplesFrom A Space Exposure Experiment: TheORGANIC Experiment on EXPOSE-R on theISSThe ORGANIC experiment on the multi-user facilityEXPOSE-R on the International Space Station investigatedthe chemical evolution, survival, destruction, and chemicalmodification of PAHs and fullerenes in space. Aromaticnetworks are among the most abundant organic material inspace. PAHs and fullerenes have been identified inmeteorites and are thought to be among the carriers fornumerous astronomical absorption and emissionfeatures.Thin films of selected PAHs and fullerenes havebeen subjected to the low Earth orbit environment as partof the ORGANIC experiment. EXPOSE-R with its experimentinserts was mounted on the outside of the ISS for 682 daysstarting in 2009. The samples were returned to Earth andinspected in spring 2011. The period outside the ISSprovided continuous exposure to the cosmic-, solar-, andtrapped-particle radiation background and >2500 h ofunshadowed solar illumination. All trays carry both solar-irradiation-exposed and dark samples shielded from the UVphotons, enabling discrimination between the effects ofexposure to solar photons and cosmic rays. The sampleswere analyzed before exposure to the space environmentwith UV-VIS and IR spectroscopy. Ground truth monitoring ofadditional sample carriers was performed through UV-VISspectroscopy at regular intervals at NASA ARC (Bryson etal. 2011, Adv. Space Res. 48, 1980). The UV-VIS and IRspectroscopic measurements were collected for thereturned flight samples. We report on the scientificexperiment, the details of the ground control analysis, andreturned flight sample results. We discuss how extendedspace exposure experiments allow to enhance ourknowledge on the evolution of organic compounds in space.Author(s): Kathryn Bryson (NASA ARC), Zan Peeters (CarnegieInstitute of Washington), Farid Salama (NASA ARC), Bernard Foing (ESA),Pascale Ehrenfreund (Space Policy Institute), Andreas Elsaesser (LeidenInstitute of Chemistry), Antonio Ricco (NASA ARC), Elmar Jessberger(Westfälische Wilhelms-Universität Münster), Addi Bischoff (WestfälischeWilhelms-Universität Münster), Michel Breitfellner (ESA), Werner Schmidt(PAH Research Institute), François Robert (Muséum National d’HistoireNaturelle)

119.07 – Dissociative Recombination ofMolecular Ions for AstrochemistryDissociative recombination (DR) of molecular ions is a keychemical process in the cold interstellar medium (ISM). DRaffects the composition, charge state, and energy balanceof such environments. Astrochemical models of the ISMrequire reliable total DR cross sections as well asknowledge of the chemical composition of the neutral DRproducts. We have systematically measured DR for manyastrophysically relevant molecular ions utilizing the TSRstorage ring at the Max-Planck-Institute for Nuclear Physics(MPIK) in Heidelberg, Germany. We used the mergedion-electron beam technique combined with an energy- andposition-sensitive imaging detector and are able to studyDR down to plasma temperatures as low as 10 K. The DRcount rate is used to obtain an absolute merged beams DRrate coefficient from which we can derive a thermal ratecoefficient needed for plasma models. Additionally wedetermine the masses of the DR products by measuringtheir kinetic energy in the laboratory reference frame. Thisallows us to assign particular DR fragmentation channelsand to obtain their branching ratios. All this information isparticularly important for understanding DR ofheteronuclear polyatomic ions. We will present DR resultsfor several ions recently investigated at TSR. A newCryogenic Storage Ring (CSR) is currently beingcommissioned at MPIK. With the chamber cooled down to

~10 K and a base pressure better than 10-13 mbar, thissetup will allow internal cooling of the stored ions down totheir rotational ground states, thus opening a new era in DRexperiments. New technological challenges arise due to theultracold, ultra-high vacuum environment of the CSR andthus the detection techniques used at TSR cannot be easilytransferred to CSR. We will present new approaches for DRfragment detection in cryogenic environment. This work issupported in part by NASA and the NSF.Author(s): Oldrich Novotny (Columbia University), A. Becker(Max-Planck-Institut für Kernphysik), H. Buhr (Weizmann Institute ofScience), Andreas Fleischmann (Universität Heidelberg), Lisa Gamer(Universität Heidelberg), W. Geppert (Stockholm University), C. Krantz(Max-Planck-Institut für Kernphysik), H. Kreckel (Max-Planck-Institut fürKernphysik), D. Schwalm (Weizmann Institute of Science), K. Spruck(Justus-Liebig-Universität Giessen), A. Wolf (Max-Planck-Institut fürKernphysik), Daniel Savin (Columbia University)

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119.08 – The Distribution, Excitation, and

Abundance of CH+ in Orion KLThe CH+ ion was one of the first molecules identified in theinterstellar gas more than 75 years ago, but its formation isstill poorly understood. The high observed abundances of

CH+ are puzzling, because the main reaction proposed for

the formation of CH+, viz., C+ + H2 ? CH+ + H, is soendothermic (4640 K), that it is unlikely to proceed at thetypical temperatures of molecular clouds. One way in whichthe high endothermicity may be overcome, is if a significantfraction of the H2 is vibrationally excited, as is the case indense molecular gas exposed to intense far-ultraviolet

radiation fields. Elucidating the formation of CH+ inmolecular clouds requires characterization of its spatialdistribution, as well as that of the key reactants in the

chemical pathways yielding CH+. Here we presenthigh-resolution spectral maps of the two lowest rotational

transitions of CH+ and the fine structure transition of C+ ina ~3?×3? region around the Orion Kleinmann-Low (KL)nebula, obtained with the Herschel Space Observatory'sHeterodyne Instrument for the Far-Infrared (HIFI). We

compare these maps to those of CH+ and C+ in the OrionBar photodissociation region (PDR), and discuss the

excitation and abundance of CH+ toward Orion KL in thecontext of chemical and radiative transfer models, whichhave recently been successfully applied to the Orion BarPDR.Author(s): Harshal Gupta (California Institute of Technology),Patrick Morris (California Institute of Technology), Zsofia Nagy (Universityof Cologne), John Pearson (California Institute of Technology)

Contributing teams: HEXOS Team

119.09 – Formation of Water on a WarmAmorphous Silicate SurfaceIt is well established that reactions on interstellar dust grainsurfaces are indispensable for water formation in space.Among all the intermediate products that lead to waterformation, the OH radical is especially important because isa product of all the three main water formation surfaceroutes, i.e., the hydrogenation of O, O2, and O3, and it alsoconnects these three routes. The desorption energy of OHfrom dust grain surfaces, along with dust graintemperature, determines the availability OH for grainsurface versus gas-phase reactions. We experimentallyinvestigated water formation on the surface of a warmamorphous silicate via H+O3?OH+O2. The surfacetemperature was kept at 50 K so as to exclude theinterference of O2. It is found that OH has a significantresidence time at 50 K. The OH desorption energy fromamorphous silicate surface is calculated to be at least 1680K, and possibly as high as 4760 K. Water is formedefficiently via OH+H and OH+H2, and the product H2Ostays on the surface upon formation. Deuterium has alsobeen used in place of hydrogen to check isotopic effects.This work is supported by NSF, Astronomy & AstrophysicsDivision (Grants No. 0908108 and 1311958) and NASA(Grant No. NNX12AF38G). We thank Dr. J.Brucato of theAstrophysical Observatory of Arcetri for providing thesamples used in these experiments.Author(s): Gianfranco Vidali (Syracuse Univ.), Jiao He (SyracuseUniv.)

119.10 – A TALE OF THREE GALAXIES:UNIQUE DUST PROPERTIES IN IRASF10398+1455, IRAS F21013-0739 AND SDSSJ0808+3948On a galactic scale the 9.7 micrometer silicate emission isusually only seen in Type 1 active galactic nuclei (AGNs).They usually also display high 5--8 micrometer emissioncontinua which are indicative of hot dust and the absenceof the polycyclic aromatic hydrocarbon (PAH) emissionbands. In contrast, starburst galaxies, luminous infraredgalaxies (LIRGs), and ultra luminous infrared galaxies(ULIRGs) exhibit a low 5--8 micrometer emissioncontinuum, a strong 9.7 micrometer silicate absorptionfeature, and strong PAH emission bands. Here we report thedetection of anomalous dust properties by Spitzer/IRS inthree galaxies (IRAS F10398+1455, IRAS F21013-0739 andSDSS J0808+3948) which are characterized by thesimultaneous detection of a low 5--8 micrometercontinuum, the 9.7 and 18 micrometer silicate emissionfeatures as well as strong PAH emission bands. The uniquedust infrared emission spectra are modeled and discussedin terms of iron-poor silicate composition, amorphouscarbon, small grain size and dust temperature in the youngAGN phase of these three galaxies.Author(s): Yanxia Xie (University of Missouri), Lei Hao (ShanghaiAstronomical Observatory, Chinese Academy of Sciences), Aigen Li(University of Missouri)

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119.11 – Laboratory Simulations of SpaceWeathering of Asteroid Surfaces by SolarWind Ions.Studies into the formation of the terrestrial planets rely onthe analysis of asteroids and meteorites. Asteroids are solarsystem remnants from the planetary formation period. Bycharacterizing their mineralogical composition we canbetter constrain the formation and evolution of the innerplanets. Remote sensing is the primary means for studyingasteroids. Sample return missions, such as Hayabusa, arecomplex and expensive, hence we rely on asteroidreflectance spectra to determine chemical composition.Links have been made and debated between meteoriteclasses and asteroid types [1, 2]. If such relationships canbe confirmed, then meteorites would provide a low costasteroid sample set for study. However, a major issue inestablishing this link is the spectral differences betweenmeteorite samples and asteroid surfaces. The mostcommonly invoked explanation for these differences is thatthe surfaces of asteroids are space weathered [2, 3]. Thedominant mechanism for this weathering is believed to besolar-wind ion irradiation [2, 4, 5]. Laboratory simulations ofspace weathering have demonstrated changes in thegeneral direction required to alter spectra fromunweathered meteorite samples to asteroid observations[3, 6 -10], but many open questions remain and we stilllack a comprehensive understanding. We propose toexplore the alleged connection of ordinary chondrite (OC)meteorites to S-type asteroids through a series ofsystematic laboratory simulations of solar-wind spaceweathering of asteroid surface materials. Here we describethe issue in more detail and describe the proposedapparatus. [1] Chapman C. R. (1996) Meteorit. Planet. Sci.,31, 699-725. [2] Chapman C. R. (2004), Annu. Rev. EarthPlanet. Sci., 32, 539-567. [3] Hapke B. (2001) J. Ge-ophys.Res., 106, 10039-10074. [4] Pieters C.M. et al. (2000)Meteorit. Planet. Sci., 35, 1101-1107. [5] Ver-nazza P. et al.(2009) Nature, 458, 993-995. [6] Stra-zulla G. et al. (2005)Icarus, 174, 31-35 (2005). [7] Brunetto R and Strazzulla G(2005) Icarus, 179, 265-273. [8] Marchi S et al. (2005)Astron. Astrophys., 443, 769-775. [9] Loeffler M. J. et al.(2009) J. Geo-phys. Res., 114, E03003. [10] Fu X. et al.(2012) Ica-rus, 219, 630-640Author(s): Kenneth Miller (Columbia University), Nathalie De Ruette(Columbia University), George Harlow (American Museum of NaturalHistory), Deborah Domingue (Planetary Science Institute), Daniel Savin(Columbia University)

119.12 – Hydrogen Implantation in Silicates:The role of solar wind in OH bond formationon the lunar surfaceAirless bodies in space such as the Moon, asteroids andinterplanetary dust particles are subject to bombardmentfrom energetic electrons and ions, ultraviolet photons,micrometeorites and cosmic rays. These bombardingparticles modify optical, chemical and physicalcharacteristics of the ices and minerals that make up thesebodies in a process known as space weathering. Inparticular, solar wind protons implanted in silicate materialscan participate in hydroxylation reactions with the oxygento form OH. This mechanism has been suggested to explaina reported 3-14% absorption signal identified as OH on thesurface of lunar soil grains and present in decreasingmagnitude from polar to equatorial latitudes. With the goal

of determining a precise OH formation rate due to H+

implantation in silicates, a series of experiments werecarried out on terrestrial minerals as analogs to lunar andinterstellar material. Experiments were carried out under

UHV pressures (<10-9 Torr) and irradiation was performedusing a mass analyzed ion accelerator. The samples werefirst outgassed to ~200 °C for 12 hrs then directlytransferred to the analysis position without exposure tolaboratory air. In-situ transmission FTIR spectroscopy wasused to determine the content of OH in thermally grownsilicon oxide and San Carlos olivine, before and after

irradiated with 1 - 5 keV H+ ions. The increase in Si-OHcontent due to irradiation was determined by subtractingthe unirradiated spectra from the irradiated spectra. Theimplanted protons induced OH stretch absorptions in the

mid-infrared peaked at 3673 cm-1 for SiO2 and 3570 cm-1

for olivine. The initial yield (OH formed per incident ion)was ~90% and the OH absorption band was found to

saturate at implantation fluences of ~2x1017 H/cm2.Irradiation also modified the Si-O stretch band at ~1090

cm-1 (9.2 ?m) causing an exponential decrease in the peakheight with increasing fluence and the appearance of a

silanol structure peaking at ~1030 cm-1. Thesemeasurements allow constraints to be placed on stellarwind contribution to observational and theoretical modelsof water on the lunar surface and on interstellar dustgrains.Author(s): Micah Schaible (University of Virginia), Raul Baragiola(University of Virginia)

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120 – Extrasolar Planet PostersPoster Session – Essex Ballroom and America Foyer – 02 Jun 2014 09:00 AM to 06:30 PM

120.01 – Performance of Transit ModelFitting in Processing Four Years of KeplerScience DataWe present transit model fitting performance of the KeplerScience Operations Center (SOC) Pipeline in processing fouryears of science data, which were collected by the Keplerspacecraft from May 13, 2009 to May 12, 2013. ThresholdCrossing Events (TCEs), which represent transiting planetdetections, are generated by the Transiting Planet Search(TPS) component of the pipeline and subsequentlyprocessed in the Data Validation (DV) component. Thetransit model is used in DV to fit TCEs and deriveparameters that are used in various diagnostic tests tovalidate planetary candidates. The standard transit modelincludes five fit parameters: transit epoch time (i.e. centraltime of first transit), orbital period, impact parameter, ratioof planet radius to star radius and ratio of semi-major axisto star radius. In the latest Kepler SOC pipeline codebase,the light curve of the target for which a TCE is generated isinitially fitted by a trapezoidal model with four parameters:transit epoch time, depth, duration and ingress time. Thetrapezoidal model fit, implemented with repeatedLevenberg-Marquardt minimization, provides a quick andhigh fidelity assessment of the transit signal. The fitparameters of the trapezoidal model with the minimumchi-square metric are converted to set initial values of thefit parameters of the standard transit model. Additionalparameters, such as the equilibrium temperature andeffective stellar flux of the planet candidate, are derivedfrom the fit parameters of the standard transit model tocharacterize pipeline candidates for the search of Earth-sizeplanets in the Habitable Zone. The uncertainties of allderived parameters are updated in the latest codebase totake into account for the propagated errors of the fitparameters as well as the uncertainties in stellarparameters. The results of the transit model fitting of theTCEs identified by the Kepler SOC Pipeline, including fittedand derived parameters, fit goodness metrics anddiagnostic figures, are included in the DV report andone-page report summary, which are accessible by thescience community at NASA Exoplanet Archive. Funding forthe Kepler Mission has been provided by the NASA ScienceMission Directorate.Author(s): Jie Li (NASA Ames Research Center), Christopher Burke(NASA Ames Research Center), Jon Jenkins (NASA Ames Research Center),Elisa Quintana (NASA Ames Research Center), Jason Rowe (NASA AmesResearch Center), Shawn Seader (NASA Ames Research Center), PeterTenenbaum (NASA Ames Research Center), Joseph Twicken (NASA AmesResearch Center)

120.02 – Revision of Earth-sized KeplerPlanet Candidate Properties with HighResolution Imaging by Hubble SpaceTelescopeIn this paper we present the first results of our HSTGO/SNAP program GO-12893 and describe how our imageanalysis using STScI's DrizzlePac software combined withour own empirical point spread function definition wereused to re-evaluate the habitability of some of the mostinteresting Kepler planet candidates. We used our highresolution imaging to calibrate Kp to the F555W and F775Wfilters on WFC3/UVIS, and spatially resolved the stellarmultiplicity of KOI-1422, KOI-2626, and KOI-3049. We foundKOI-1422 to be a tight binary star system with a projectedseparation of 0.217’’ (~90 AU). We found KOI-2626 to be atriple star system with a projected separation of 0.201’’(~110 AU) between the primary and secondarycomponents and 0.161’’ (~90 AU) between the primary andtertiary components. We found KOI-3049 to be a binary starsystem with a projected separation of 0.464’’ (~330 AU).Using theoretical isochrones from the Dartmouth StellarEvolution Database, we performed hierarchical fitting usingour derived photometry and the synthetic photometry fromthe isochrones. Revised stellar parameters for theindividual components of the systems show that the starsin these systems range from early-K dwarf to early-M dwarfspectral types. We report with high confidence that all threesystems are bound and co-eval based on the tightisochrone fitting and false positive analysis. Using ourbest-fit stellar parameters from the isochrone matches, wesolved for the properties of the planets in the three systemsand found that the planets range in size from ~2REarth to~4 REarth, placing them in the Super Earth/mini-Neptunerange. Some planets analyzed here are potentiallyhabitable depending on their stellar host and greenhouseeffect level.Author(s): Kimberly Star (The Center for Exoplanets and HabitableWorlds), Ronald Gilliland (The Center for Exoplanets and HabitableWorlds)

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120.03 – Characterizing the TransitingPlanet Search of the Kepler Data ProcessingPipelineThe Kepler Mission continuously observed a host of targetstars, for over four years, in a 115 square-degree field ofview to discover Earth-like planets transiting Sun-like starsthrough analysis of photometric data. The Kepler ScienceOperations Center at NASA Ames Research Centerprocesses the data from the Kepler spacecraft with theScience Processing Pipeline, which is composed of severalmodules including the Transiting Planet Search (TPS). Inorder to accomplish the primary goal of the mission,computing the fraction of stars containing potentiallyhabitable Earth-like planets, it is critical to understand anybiases that the data processing imposes on the results.Currently, a massive effort to characterize this ScienceProcessing Pipeline is underway. An infrastructure forcharacterizing TPS, through the injection of artificial signals,has been built and is being used to understand ourdetection probability on a large set of "quiet" targets. Thisinfrastructure will enable us to understand the factors thataffect detectability such as signal strength, orbital period,host-star type, galactic latitude, etc. Here we present theresults of an initial study focused on a quiet set of targets,with hundreds of injections in each, using the first fouryears of data collected by Kepler.Author(s): Shawn Seader (SETI), Peter Tenenbaum (SETI), ChristopherBurke (SETI), Jon Jenkins (NASA Ames Research Center)

120.04 – Finding Every Planet We Can --Removal of Transit-like False Triggers inKepler Data.With the Kepler data set now extant at 4 years, evengreater pressure is placed on the processing pipeline to ekeout every last transit signal in the data. Central to this endis the reduction of false positives during transit searching. Alarge fraction of the false positives are due to individualsystematic spike events in the data. Various veto methodsare utilized to remove these false positives butnevertheless, their presence risks to mask true planetsignatures. A systematic spike remover has beendeveloped in the Presearch Data Conditioning (PDC)component of the Kepler pipeline which removes shortsystematic spikes in the target light curves. This reducesfalse positives which not only increases the likelihood ofdetecting real transiting planets, but also improves theefficiency of running the pipeline and vetting of the results.Author(s): Jeffrey Smith (NASA Ames Research Center), JosephCatanzarite (NASA Ames Research Center), Shawn Seader (NASA AmesResearch Center), Jon Jenkins (NASA Ames Research Center)

120.06 – Recent Developments in KeplerPipeline Data ValidationLight curves for the vast majority of Kepler targets aresearched for transiting planet signatures in the TransitingPlanet Search (TPS) component of the Science OperationsCenter (SOC) Processing Pipeline. Targets for which thedetection threshold is exceeded are subsequentlyprocessed in the Data Validation (DV) Pipeline component.The primary functions of DV are to (1) characterize planetsidentified in the transiting planet search, (2) search foradditional transiting planet signatures in light curves aftertransit signatures have been removed, and (3) perform acomprehensive suite of diagnostic tests to aid indiscrimination between true transiting planets and falsepositive detections. DV output products include extensivereports by target, one-page report summaries by planetcandidate, and tabulated planet model fit and diagnostictest results. The Q1-Q16 Kepler data set was processedwith TPS/DV (SOC release 9.1) in August 2013. Transitingplanet detections and DV products were delivered to theExoplanet Archive at the NASA Exoplanet Science Institute(NExScI). We describe developments in Data Validation thathave been introduced in the Pipeline codebase subsequentto SOC 9.1. We have enhanced diagnostic test functionalityto improve the performance of (human and automated)planet candidate vetting processes that rely on DVproducts; this necessarily increases the reliability of Keplerplanet catalogs. We have also updated the report andsummary products that are archived for the community andshall remain a significant part of the Kepler legacy. Weillustrate the recent developments with examples fromTPS/DV processing of the full Q1-Q17 Kepler data set. Someof the developments we describe were released with SOC9.2 in March 2014; others have been introduced later intothe SOC codebase and will be released with SOC 9.3. TheExoplanet Archive is located atexoplanetarchive.ipac.caltech.edu. Funding for the KeplerMission has been provided by the NASA Science MissionDirectorate.Author(s): Joseph Twicken (NASA Ames Research Center), BruceClarke (NASA Ames Research Center), Forrest Girouard (NASA AmesResearch Center), Jon Jenkins (NASA Ames Research Center), Todd Klaus(NASA Ames Research Center), Jie Li (NASA Ames Research Center), SeanMcCauliff (NASA Ames Research Center), Elisa Quintana (NASA AmesResearch Center), Shawn Seader (NASA Ames Research Center), PeterTenenbaum (NASA Ames Research Center), Natalie Batalha (NASA AmesResearch Center), Steve Bryson (NASA Ames Research Center),Christopher Burke (NASA Ames Research Center), Douglas Caldwell (NASAAmes Research Center), Jason Rowe (NASA Ames Research Center)

Contributing teams: Kepler Science Operations Center,Kepler Science Office

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120.07 – Rolling Band Artifact Flagging inthe Kepler Data PipelineInstrument-induced artifacts in the raw Kepler pixel datainclude time-varying crosstalk from the fine guidancesensor (FGS) clock signals, manifestations of drifting moirépattern as locally correlated nonstationary noise and rollingbands in the images. These systematics find their way intothe calibrated pixel time series and ultimately into thetarget flux time series. The Kepler pipeline moduleDynablack models the FGS crosstalk artifacts using acombination of raw science pixel data, full frame images,reverse-clocked pixel data and ancillary temperature data.The calibration module (CAL) uses the fitted Dynablackmodels to remove FGS crosstalk artifacts in the calibratedpixels by adjusting the black level correction per cadence.Dynablack also detects and flags spatial regions and timeintervals of strong time-varying black-level. These rollingband artifact (RBA) flags are produced on a per row percadence basis by searching for transit signatures in theDynablack fit residuals. The Photometric Analysis module(PA) generates per target per cadence data quality flagsbased on the Dynablack RBA flags. Proposed future workincludes using the target data quality flags as a basis forde-weighting in the Presearch Data Conditioning (PDC),Transiting Planet Search (TPS) and Data Validation (DV)pipeline modules. We discuss the effectiveness of RBAflagging for downstream users and illustrate with someaffected light curves. We also discuss the implementationof Dynablack in the Kepler data pipeline and present resultsregarding the improvement in calibrated pixels and theexpected improvement in cotrending performance as aresult of including FGS corrections in the calibration.Funding for the Kepler Mission has been provided by theNASA Science Mission Directorate.Author(s): Bruce Clarke (SETI Institue), Jeffery Kolodziejczak (NASAMSFC), Douglas Caldwell (SETI Institue)

Contributing teams: Kepler Science Operations Center,Kepler Science Office

120.08 – Improving Kepler PipelineSensitivity with Pixel Response FunctionPhotometry.We present the results of our investigation into thefeasibility and expected benefits of implementingPRF-fitting photometry in the Kepler Science ProcessingPipeline. The Kepler Pixel Response Function (PRF)describes the expected system response to a point sourceat infinity and includes the effects of the optical pointspread function, the CCD detector responsivity function,and spacecraft pointing jitter. Planet detection in the Keplerpipeline is currently based on simple aperture photometry(SAP), which is most effective when applied to uncrowdedbright stars. Its effectiveness diminishes rapidly as targetbrightness decreases relative to the effects of noise sourcessuch as detector electronics, background stars, and imagemotion. In contrast, PRF photometry is based on fitting anexplicit model of image formation to the data and naturallyaccounts for image motion and contributions of backgroundstars. The key to obtaining high-quality photometry fromPRF fitting is a high-quality model of the system's PRF,while the key to efficiently processing the large number ofKepler targets is an accurate catalog and accurate mappingof celestial coordinates onto the focal plane. If the CCDcoordinates of stellar centroids are known a priori then theproblem of PRF fitting becomes linear. A model of theKepler PRF was constructed at the time of spacecraftcommissioning by fitting piecewise polynomial surfaces todata from dithered full frame images. While this modelaccurately captured the initial state of the system, the PRFhas evolved dynamically since then and has been seen todeviate significantly from the initial (static) model. Weconstruct a dynamic PRF model which is then used torecover photometry for all targets of interest. Bothsimulation tests and results from Kepler flight datademonstrate the effectiveness of our approach. Kepler wasselected as the 10th mission of the Discovery Program.Funding for this mission is provided by NASA’s ScienceMission Directorate. Kepler was selected as the 10thmission of the Discovery Program. Funding for this missionis provided by NASA’s Science Mission Directorate.Author(s): Robert Morris (NASA Ames Research Center), SteveBryson (NASA Ames Research Center), Jon Jenkins (NASA Ames ResearchCenter), Jeffrey Smith (NASA Ames Research Center)

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120.09 – Automatic Classification of KeplerThreshold Crossing EventsOver the course of its 4-year primary mission the Keplermission has discovered numerous planets. Part of theprocess of planet discovery has involved generatingthreshold crossing events (TCEs); a light curve with arepeating exoplanet transit-like feature. The large numberof diagnostics (~100) makes it difficult to examine all theinformation available for each TCE. The effort required forvetting all threshold-crossing events (TCEs) takes severalmonths by many individuals associated with the KeplerThreshold Crossing Event Review Team (TCERT). The totalnumber of objects with transit-like features identified in thelight curves has increased to as many as 18,000, justexamining the first three years of data. In order toaccelerate the process by which new planet candidates areclassified, we propose a machine learning approach toestablish a preliminary list of planetary candidates rankedfrom most credible to least credible. The classifier mustdistinguish between three classes of detections:non-transiting phenomena, astrophysical false positives,and planet candidates. We use random forests, asupervised classification algorithm to this end. We report onthe performance of the classifier and identify diagnosticsthat are important for discriminating between these classesof TCEs. Funding for this mission is provided by NASA’sScience Mission Directorate.Author(s): Sean McCauliff (NASA Ames Research Center), JosephCatanzarite (Orbital Science Corporatin), Jon Jenkins (Orbital ScienceCorporatin)

120.10 – The NASA Exoplanet Archive: DataInventory ServiceWe present here the latest addition to the NASA ExoplanetArchive - the Data Inventory Service, a tool aimed toprovide the user with all the data available within thearchive (exoplanet and stellar parameters, time series fromground-based transit surveys (such as Super WASP, XO,HAT-P, KELT), Kepler Pipeline products, CoRoT light curves,etc.) at or near the location of an astronomical object. TheNASA Exoplanet Archive is an online service dedicated tocompile and to serve public astronomical data sets involvedin the search for and characterization of extrasolar planetsand their host stars. The data in the archive include stellarparameters (e.g., positions, magnitudes, temperatures,etc.), exoplanet parameters (such as masses and orbitalparameters) and discovery/characterization data (e.g.,published radial velocity curves, photometric light curves,spectra, etc.). In support of the Kepler Extended Mission,the NASA Exoplanet Archive also hosts data related toKepler Objects of Interest (KOI), Kepler Pipeline productssuch as Threshold Crossing Events (TCE) and DataValidation Reports, and Kepler Stellar parameters as usedby the Kepler Pipeline. The archive provides tools to workwith these data, including interative tables (with plottingcapabilities), interactive light curve viewer, periodogramservice, transit and ephemeris calculator, and applicationprogram interface. To access this information visit us at:http://exoplanetarchive.ipac.caltech.eduAuthor(s): Solange Ramirez (Caltech), Rachel Akeson (Caltech), DavidCiardi (Caltech), Xi Chen (Caltech), Jessie Christiansen (Caltech), PeterPlavchan (Caltech)

Contributing teams: NASA Exoplanet Archive Team

120.11 – What Can The Habitable ZoneGallery Do for You?The Habitable Zone Gallery (www.hzgallery.org) has beenonline since August 2011 as a service to the exoplanetcommunity to provide Habitable Zone (HZ) information foreach of the exoplanetary systems with known planetaryorbital parameters. The service includes a sortable table, aplot with the period and eccentricity of each of the planetswith respect to their time spent in the HZ, a gallery ofknown systems which plots the orbits and the location ofthe HZ with respect to those orbits, and orbital movies.Recently, we have added new features including:implementation of both conservative and optimistic HZs,more user-friendly table and movies, movies forcircumbinary planets, and a count of planets whose orbitslie entirely within the system’s HZ. Here we discuss variouseducational and scientific applications of the site such astarget selection, exploring planets with eccentric orcircumbinary orbits, and investigating habitability.Author(s): Dawn Gelino (NASA Exoplanet Science Institute,Caltech), Stephen Kane (San Francisco State University)

120.12 – Stellar Activity Masking andMimicking Habitable ExoplanetsFuture generations of precise radial velocity (RV) surveysaim to attain a sensitivity sufficient to detect Earth massplanets orbiting in their host star's habitable zones. The RVsemi-amplitude of such a planet can be significantlysmaller than RV variations caused by stellar "jitter". SomeRV variations, in particular those caused by starspotsrotating in and out of view and those caused by magneticactivity cycles can be periodic in nature and can mimicplanetary RV signals. We calculate and compare therelative timescales and amplitudes of RV variations due toactivity and habitable planetary companions as a functionof stellar mass, and discuss the ramifications for RVsurveys.Author(s): Andrew Vanderburg (Harvard University), Peter Plavchan(Infrared Processing and Analysis Center), John Johnson (HarvardUniversity)

120.13 – Characterization of thePerformance of MANIC, a MonolithicAchromatic Nulling InterferenceCoronagraphWe present the characterization of the performance of amonolithic achromatic nulling interference coronagraph(MANIC). The primary scientific goal of this instrument is todirectly image inner exoplanetary environmentssurrounding stars. The nulling performance of theinstrument is optimized through use of wave front sensingand control. The measurement of the null and theinstrument’s limiting factors are presented with this poster.Author(s): Kathleen Oram (University of Massachusetts Lowell),Timothy Cook (UMLCAR), Supriya Chakrabarti (UMLCAR), Brian Hicks(UMLCAR)

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120.14 – ACCESS: The Arizona-CfA-CatolicaExoplanet Spectroscopy SurveyThe Arizona-CfA-Catolica Exoplanet Spectroscopy Survey(ACCESS) is an international, multi-institutional consortiumwith members from the Harvard-Smithsonian CfA, theUniversity of Arizona, Pontificia Universidad Catolica inChile, MIT and UC Santa Cruz and the Carnegie Institution.ACCESS' goal is to observe about two dozen planetscovering a wide range of mass, radius, atmospherictemperatures and energy irradiation levels, with two mainscientific goals: 1) to obtain, for the first time, a uniformsample of visible transmission spectra of exoplanets,allowing the study of their atmospheric characteristics as astatistically significant sample, and 2) to mature thetechnique of ground-based observations of exoplanetaryatmospheres for future observations of small planets. Herewe describe ACCESS and its first science results.Author(s): Mercedes Lopez-Morales (Harvard-Smithsonian CfA),Daniel Apai (University of Arizona), Andres Jordan (Pontificia Universidadcatolica), Nestor Espinoza (Pontificia Universidad catolica), BenjaminRackham (University of Arizona), Jonathan Fraine (Pontificia Universidadcatolica), Florian Rodler (Harvard-Smithsonian CfA), Nikole Lewis(Massachusetts Institute of Technology), Jonathan Fortney (University ofCalifornia, Santa Cruz), David Osip (Observatories of the CarnegieInstitution for Science)

120.15 – The MEarth Project: Status Updateand the Commissioning of a Brand NewTelescope Array in the SouthernHemisphereThe MEarth Project is an ongoing all-sky survey forEarth-like planets transiting the closest, smallest M dwarfs.MEarth aims to find good targets for atmosphericcharacterization with JWST and the next generation ofenormous ground-based telescopes. MEarth's yearly datareleases, containing precise light curves of nearbymid-to-late M dwarfs, provide a unique window into thephotometric variability of the stars that will forever beamong the most interesting targets in the search forpotentially habitable exoplanets. We present a statusupdate on the MEarth Project, including a detailed map ofthe progress we’ve made so far with 8 telescopes in theNorthern hemisphere and promising early results from ournew installation of 8 more telescopes in the Southernhemisphere.Author(s): Zachory Berta-Thompson (MIT), Jonathan Irwin(Smithsonian Astrophysical Observatory), David Charbonneau (HarvardUniversity), Elisabeth Newton (Harvard University), Jason Dittmann(Harvard University)

120.16 – The Impact of Stellar Multiplicityon Planet OccurrenceThe majority of searches for extrasolar planets haveconcentrated exclusively on single stars, actively avoidingclose binary systems where the companion mightcomplicate the observations and data analysis. However,the major ity of solar-type stars are found in binarysystems. These binary companions should exert a strongdynamical influence on any planetary system, and hencethis systematic bias leaves out knowledge of planetformation fundamentally incomplete. We will present theongoing results of a high-resolution imaging survey toidentify binary companions among a volume-limited sampleof 600 Kepler planet hosts within 500 parsecs. This surveyexploits nonredundant aperture-mask interferometry (NRM)to super-resolve binary companions down to 1/4 of thediffraction limit (15 mas; <5 AU at 300 pc), identifying thedynamically significant binary companions that are missedby standard imaging surveys. Our results show that binaritydoes indeed have a profound influence on planetoccurrence, suppressing the planet frequency by a factor of4 in 5-50 AU binaries. However, unexpected trends forplanet survival also are starting to emerge.Author(s): Adam Kraus (UT - Austin), Michael Ireland (ANU), AndrewMann (UT - Austin), Daniel Huber (NASA Ames), Trent Dupuy (UT - Austin)

120.17 – Orbital Stability Analysis of GJ 581and HD 10180We present self-consistent orbital stability results over 107

years for GJ 581 for models including planets b, c, d, e, andg. We find substantial overlap between constraints onstability for planet e and its radial velocity-derivedparameters. We find a smaller overlap between constraintsof stability and RV fit for planet g, however not so small asto rule out planet g on stability requirements alone. Weperform an F-test on RV fit results with and without planet gsubject to the condition of orbital stability and do not findsignificant evidence for the existence of GJ 581 g givencurrent radial velocity data. We also apply the process toHD 10180 to investigate the stability of 9 planets that havebeen reported in this system, and present results related tothe stability of proposed planet HD 10180 i.Author(s): David Joiner (Kean University), Cesar Sul (San Jose StateUniversity), Diana Dragomir (UC Santa Barbara), Stephen Kane (SanFrancisco State University), Monika Kress (San Jose State University),Kimberly Shanks (Kean University)

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120.18 – Giant Planet Accretion in aLow-Turbulence Circumplanetary DiskAt least 5% of confirmed planets discovered by the KeplerMission have a mass greater than Jupiter's. Gas giants moremassive than Saturn account for at least 18% of allconfirmed planets.The final stages of gas accretion of agiant planet occur in the presence of a circumplanetarydisk (CPD). Recently, it was proposed that turbulence (andhence transport) in these disks is driven by MRI, possiblygenerating low-turbulence regions known as Dead Zones. Itwas thus suggested that gas accretion through a CPD andon the planet can be severely reduced by a Dead Zone. IfCPDs create a bottleneck for the accretion of gas, then thegrowth of planets more massive than Jupiter may becomeproblematic. We investigate how gas accretion on aJupiter-mass planet is affected by a Dead Zone by means ofglobal 3D hydrodynamics calculations. We model both theCPD and the protoplanetary disk. The accretion flow isresolved at a length scale smaller than Jupiter's radius, Rj,by using a nested-grid technique. We assume that thekinematic viscosity is constant and equal to nu=1e-5Omega a^2, where a and Omega are respectively theplanet's orbital radius and frequency. A Dead Zone aroundthe planet is represented by a region of low viscosity(nu=1e-8 Omega a^2), extending out to ~60Rj and aboveand below the CPD mid-plane for a few local scale heights.We obtain an accretion rate of ~5e-5 Omega Sigma a^2,where Sigma is the unperturbed protoplanetary diskdensity. Calculations by D'Angelo et al. (2003) and Bate etal. (2003), which used nu=1e-5 Omega a^2 everywherebut applied a much coarser resolution and differentaccretion parameters, found an accretion rate of ~2e-4Omega Sigma a^2. Accounting for variations of severaltens of percent, arising from differences (between theseand previous calculations) in numerical parameters andresolution, we argue that a CPD Dead Zone, as modeledhere, does not significantly affect the gas accretion rate ofa giant planet. This result is compatible with severalprevious studies, which found that the accretion flowinvolves mostly gas at and above the CPD surface.Continued accretion in the presence of a CPD is alsoconsistent with observed exoplanets several times moremassive than Jupiter.Author(s): Gennaro D'Angelo (SETI Institure), Francesco Marzari(University of Padova)

120.19 – Visual Companions to TransitingHot JupitersThe known short period giant planets constitute a valuablestatistical population. From the derived physical and orbitalproperties of this sample in conjunction with detailedstudies of individual objects, we can investigate a widearray of topics, including the internal structures of giantplanets, the conditions under which planets form, and theirdynamical evolution. The success of such studies relies, ofcourse, on the completeness and accuracy of theunderlying data, but many of the known hot Jupiters havenot been subjected to high resolution imaging in search ofclose stellar companions. The presence of a second star(whether physically bound or a chance alignment), canaffect the derived stellar and planetary parameters.Moreover, the presence of bound companions can inform usabout planetary formation and migration in binary systems.Here we present preliminary results from our adaptiveoptics survey of 94 transiting hot Jupiter host stars anddiscuss their significance in the context outlined above.Author(s): Samuel Quinn (Georgia State University), Lars Buchhave(Harvard-Smithsonian Center for Astrophysics), Russel White (GeorgiaState University), Deepak Raghavan (Georgia State University)

120.20 – Untangling Planet Signals andStellar Noise with Precision Radial VelocityMeasurementsRadial velocity instrumental precision has improved to thedegree that measurements are now partially limited by thenoise intrinsic to the host star, or stellar ‘jitter’. Severaldifferent phenomena contribute to the observed jitter,including pressure waves, granulation, magnetic featurescaused by stellar activity, and solar-like magnetic cycles.The amplitude of these effects ranges from 10 to 400 cm/s,depending on stellar type, and pose a significant limitationto detecting Earth analogues. We analyze two years ofradial velocity data from a survey of bright, quiet stars withthe HARPS-N instrument, an ultra-stabilized R=115,000cross-dispersed spectrograph located on the 3.6mTelescopio Nazionale Galileo on the island of La Palma. Welook for correlations between these RV measurements andknown activity indicators, including line bisectormeasurements and the CaII index. We also investigate thecorrelation between radial velocity measurements andother spectral variations, including equivalent widths offeatures selected by a blind search. By fitting for theseeffects simultaneously, we can improve the radial velocityprecision, enabling the detection of low-mass planets.Author(s): Sara Gettel (Harvard-Smithsonian Center forAstrophysics), David Charbonneau (Harvard-Smithsonian Center forAstrophysics)

Contributing teams: the HARPS-N Collaboration

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120.21 – "Rare" Microlensing Events: howfrequent are they? what can they teach us?Today's microlensing teams discover roughly 2000candidate microlensing events per year. Many of theseexhibit the standard point-source/point-lens form, and arecaused by distant lenses we cannot detect. In our posterwe report on the preliminary results of a long term programof analysis designed to identify and study "rare"gravitational lensing events. We have focused on those rareevents with light curve profiles that differ from the point-source/point-lens form. These unusual light curves provideadditional information about the lens or source. We devotespecial effort to the study of a small set of events thatappear to have been caused by nearby lenses. Nearbylenses are interesting, whatever the form of the light curvethey generate. We show that some unusual events arecommon enough that their systematic study can bescientifically fruitful, allowing lensing programs to identifynearby (closer than a kiloparsec) compact objects andmeasure their masses, and to also identify and measuremasses in nearby planetary systems. We have developedmethods that should prove useful in a wide range ofground-based and space-based lensing studies.Author(s): Rosanne Di Stefano (Harvard-Smithsonian CfA), WilliamBryk (Ramaz Upper School), Idan Ginsburg (Harvard-Smithsonian CfA),Jochen Greiner (MPE), Sebastien Lepine (Georgia State University), AntoniaOprescu (Harvard-Smithsonian CfA), Francis Primini (Harvard-SmithsonianCfA), Ben Tunbridge (Harvard-Smithsonian CfA)

120.22 – Open Source Cloud Computing forTransiting Planet DiscoveryWe provide an update on the development of theopen-source software suite designed to detect exoplanettransits using high-performance and cloud computingresources (https://github.com/openEXO). Our collaborationcontinues to grow as we are developing algorithms andcodes related to the detection of transit-like events,especially in Kepler data, Kepler 2.0 and TESS data whenavailable. Extending the work of Berriman et al. (2010,2012), we describe our use of the XSEDE-Gordonsupercomputer and Amazon EMR cloud to search foraperiodic transit-like events in Kepler light curves. Suchevents may be caused by circumbinary planets or transitingbodies, either planets or stars, with orbital periodscomparable to or longer than the observing baseline suchthat only one transit is observed. As a bonus, we use thesame code to find stellar flares too; whereas transits reducethe flux in a box-shaped profile, flares increase the flux in afast-rise, exponential-decay (FRED) profile thatnevertheless can be detected reliably with a square-wavefinder.Author(s): Peter McCullough (Johns Hopkins), Scott Fleming (STScI),Andrea Zonca (San Diego Supercomputer Center), Jack Flowers (ReedCollege), Duy Cuong Nguyen (University of Toronto), Robert Sinkovits (SanDiego Supercomputer Center), Pavel Machalek (Johns Hopkins Alumni)

120.23 – Structure and Dynamics of ColdWater Super-Earths: The Case of OccludedCH4 and its OutgassingIn this work we study the transport of methane in theexternal water envelopes surrounding water-rich super-Earths. We investigate the influence of methane on thethermodynamics and mechanics of the water mantle. Wefurther explore the dynamics of possible tectonic modesactive in these planets and derive overturn and resurfacingtime scales as a function of ice mass fraction. We propose amechanism for methane release into the atmosphere andformulate the relation between the outgassing flux and thetectonic mode dynamical characteristics. We givenumerical estimates for the global outgassing rate ofmethane into the atmosphere. We suggest a qualitativeexplanation for how the same outgassing mechanism mayresult in either a stable or a runaway volatile release,depending on the specifics of a given planet.Author(s): Amit Levi (Harvard-Smithsonian Center forAstrophysics), Dimitar Sasselov (Harvard-Smithsonian Center forAstrophysics), Morris Podolak (Tel-Aviv University)

120.24 – Implications of CME Deflections onthe Habitability of Planets Around M DwarfsSolar coronal mass ejections (CMEs) are known to produceadverse space weather effects at Earth. These effectsinclude geomagnetically induced currents and energeticparticles accelerated by CME-driven shocks. Significantnon-radial motions are observed for solar CMEs with theCME path deviating as much as 30 degrees within 20 solarradii. We have developed a model, Forecasting a CME'sAltered Trajectory (ForeCAT), which predicts the deflectedpath of a CME according to the magnetic forces of thebackground solar wind. In Kay et al (2013), we show thatthese magnetic forces cause CMEs to deflect towards theregion of minimum magnetic field strength. For the Sun,this magnetic minimum corresponds to the HeliosphericCurrent Sheet (HCS). We predict that the Earth is mostlikely to be impacted by a deflected CME when its orbitbrings it near the HCS. M dwarfs can have magnetic fieldstrengths several orders of magnitude larger than the Sunwhich will strongly affect CME deflections. We explorestellar CME deflections with ForeCAT. We present results forM4V star V374 Peg. We determine potential impacts causedby CME deflections for a planet located within the habitablezone of V374 Peg (~20-40 solar radii). We discuss futureextensions as including variations in solar cycle, capturingsmall structures such as active regions, and extensions forother M dwarf stars.Author(s): Christina Kay (Boston Univ.), Merav Opher (Boston Univ.)

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120.25 – Road Testing AsterodensityProfiling using Flicker as an InputAsterodensity Profiling (AP) is a young but powerful tool forstudying transiting exoplanets. A transit light curve directlyreveals the mean stellar density, under various idealizedassumptions such as circular orbits and no blended light.By comparing this observed density to some independentmeasure, differences (or lack there-of) can be used toextract useful information on particular systems, such asthe orbital eccentricity and the amount of blended light. Ina previous paper, we were able to use AP to infer a highfalse rate for the KOIs of giant stars (Sliski & Kipping 2014)by using asteroseismology as the independent measure.Recently, the analysis of brightness variations on an 8-hourtimescale ("flicker") has emerged as a less precise butmore widely applicable alternative method for deriving astar's density. Here, we road-test the flicker technique onthe 41 KOIs studied previously, to test whether our previousconclusion of a high giant star false positive rate can berecovered using flicker alone. Secondly, we explore thepossibility of extending AP to hundreds of Kepler targets,where generally flicker remains viable but asteroseismologydoes not. Finally, we discuss the impact of this technique tofuture missions such as TESS and PLATO missions, with aview to both planet validation and extracting theeccentricity distribution of different planet populations.Author(s): David Sliski (Harvard-Smithsonian Center forAstrophysics ), David Kipping (Harvard-Smithsonian Center forAstrophysics )

120.26 – Reconnaissance of Stars withinTwenty-Five Parsecs: Red Dwarfs Rule theGalaxyThe REsearch Consortium On Nearby Stars (RECONS,www.recons.org) team has been mapping the solarneighborhood for 20 years. We continue to collect originalastrometric, photometric, and spectroscopic data for thenearest stars and their companions, with significant effortconcentrated in the southern hemisphere at the CTIO 0.9mtelescope, operated by RECONS for the SMARTSConsortium. These new data are combined with carefullyvetted data from classic surveys to paint the mostcomplete portrait to date for the nearby stars. Thecombined data from RECONS and others have beenorganized into the RECONS 25 Parsec Database, which asof January 1, 2014 includes 3074 stars, brown dwarfs, andexoplanets in 2168 systems. All of these systems haveaccurate trigonometric parallaxes in the refereed literatureplacing them closer than 25.0 parsecs, i.e. parallaxesgreater than 40 mas with errors less than 10 mas.Statistical results from this comprehensive Database areoutlined, allowing us to make an unprecedented census ofthe Galaxy's stellar population, of which more than three-quarters are red dwarfs. Fewer than twenty of these reddwarfs are currently known to harbor planets, indicatingthat a great deal of work remains to be done in the searchfor the nearest worlds outside our Solar System. It isvirtually certain that most planets in the Galaxy are orbitingred dwarfs, and the nearest examples should be among theprime targets in our search for life elsewhere. This efforthas been supported by the NSF through grantsAST-0908402 and AST-1109445, and via observations madepossible by the SMARTS Consortium.Author(s): Todd Henry (RECONS), Wei-Chun Jao (Georgia StateUniversity), Tiffany Pewett (Georgia State University), Adric Riedel (HunterCollege/AMNH), Justin Rodriguez (Georgia State University), MicheleSiverstein (Georgia State University), Kenneth Slatten (RECONS), JenniferWinters (Georgia State University)

Contributing teams: RECONS

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121 – Pulsars, Neutron Stars, and Supernovae PostersPoster Session – Essex Ballroom and America Foyer – 02 Jun 2014 09:00 AM to 06:30 PM

121.01 – Low Mach Number Simulations ofNuclear Flames Using Spectral DeferredCorrectionsMany phenomena in Astrophysics are largely subsonic andrequire special techniques for long-time integration.MAESTRO is a low Mach number stellar hydrodynamicscode that can be used to simulate long-time, low-speedflows that would be extremely time consuming to simulateusing traditional compressible codes. MAESTRO filterssound waves while retaining both local and large-scalecompressibility which gives increased accuracy andefficiency. In this project we describe the results of applyingMAESTRO to thermonuclear flames (thin propagatingthermonuclear fusion fronts) as well as the convective layerof a nova. The nova is a carbon-oxygen white dwarf with ahydrogen-helium envelope in tight hydrostatic equilibrium.As the envelope increases in mass, the pressure andtemperature increase at the base of the accreted layer.When the pressure and temperature are sufficiently high,nuclear fusion (burning) occurs. To capture this burning, weuse the extensive reaction network of the Modules forExperiments in Stellar Astrophysics (MESA) code to modelthe reactions in the flow. We apply a spectral deferredcorrections (SDC) algorithm to couple the reactions to thehydrodynamics. We present the results of applying the SDCtemporal integration strategy in low Mach numbersimulations of thermonuclear flames. The SDC approachprovides a better coupling between the various physicalprocesses with greater accuracy and reducedcomputational cost as compared to a Strang splittingapproach. This work was supported in part by a DOE/Officeof Nuclear Physics grant No. DE-FG02-06ER41448 to StonyBrook.Author(s): Ryan Orvedahl (University of Colorado at Boulder ),Michael Zingale (Stony Brook University), Ann Almgren (Lawrence BerkeleyNational Laboratory), John Bell (Lawrence Berkeley National Laboratory),Andrew Nonaka (Lawrence Berkeley National Laboratory)

121.02 – The Earliest Type Oe Stars:Shattering the Record for the BePhenomenonOe stars are massive and likely evolved stars that may bekey to understanding aspects of massive star evolution.These are rapidly rotating stars that may have spun upduring main sequence evolution and are believed to haveformed decretion disks. A decretion disk forms when stellarmaterial is spun out of a star as it rotates near break-upvelocity. Oe stars are extremely rare in the Milky Way (MW),where the earliest known Oe star has a spectral type ofO7.5. Because weaker stellar winds prevent O stars fromlosing angular momentum, this model of Oe disk formationpredicts that, in low metallicity environments, the weakwinds allow larger numbers and frequencies of early-typeOe stars. We test this scenario in the low-metallicity, SmallMagellanic Cloud (SMC), where we have identifiedapproximately 30 field Oe stars from RIOTS4, a spatiallycomplete, spectroscopic survey of field OB stars. To date,the earliest reported Oe star in any galaxy is type O7.5.However, here we find seven Oe stars of types O5 to O7,thus yielding much earlier type Oe stars than ever before.Therefore, the increase in the frequency of early-type Oestars in the SMC compared to the MW supports thedecretion disk model because the weaker winds inlow-metallicity environments allow earlier type O stars toform decretion disks. Funding for this project was providedby NSF grant AST-0907758.Author(s): Jesse Golden-Marx (University of Michigan), M. Oey(University of Michigan), Joel Lamb (Nassau Community College), AndrewGraus (University of California, Irvine)

121.03 – Infrared Spectral EnergyDistributions of Nearby Dwarf Carbon StarsThe discovery of G77?61 (Dahn et al. 1977) -- a star with acarbon-rich spectrum a mere 58 pc away and therefore ofrelatively low luminosity -- led to the recognition that_dwarf_ carbon (dC) stars exist. As more dCs are nowknown, the accepted paradigm of the presence ofatmospheric carbon is that dCs must contain a white dwarfsecondary. While the white dwarf companion was goingthrough an AGB stage, it deposited carbon-rich material inthe atmosphere of the lower-mass (and now brighter) dwarfstar. Indeed, a handful of the dC's have exhibited radialvelocity signatures consistent with this picture. To allow forthe carbon to still be present in the atmosphere past theAGB stage, a replenishing outer shell or disk has beenproposed. Current understanding of the formation andevolution of a dC is, however, limited by the small numberof objects and observations. We present a full range offluxes and flux limits from 1 - 160 um including 2MASS,WISE, Spitzer, and Herschel observations for a list of thenearest carbon dwarfs. We reconstruct the spectral energydistribution exploring the mid-infrared region where anyresidual debris disks would be detectable. The carbondwarfs have been historically studied in the visible, andthese new infrared observations provide a picture of thecircumstellar dust.Author(s): Patrick Lowrance (Spitzer Science Center/Caltech)

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121.04 – Atomic Hydrogen in the ExtendedCircumstellar Envelope of the Carbon StarIRC+10216IRC+10216 (CW Leo) is the nearest and best-known carbonstar. It is currently undergoing a high rate of mass loss

(~10-5 M? yr-1) and is believed to be approaching the endof its lifetime on the asymptotic giant branch. Mass lossfrom IRC+10216 has led to the formation of an extensivecircumstellar envelope (CSE) that spans more than half adegree (>1.3 parsecs) across and is both structurally andchemically complex. While the CSE of IRC+10216 has beenwidely studied through emission from dust and molecularlines, the properties of the predominant CSE constituent—hydrogen gas—have remained poorly known, includingthe total mass and extent of the circumstellar hydrogenand the ratio of atomic to molecular hydrogen throughoutthe envelope. I will present new insights into thesequestions based on a study of IRC+10216 in the HI 21-cmline using the Very Large Array and the Robert C. ByrdGreen Bank Telescope. I will also highlight the value of HIline emission as a probe of the interface between thecircumstellar and interstellar environment of the star.Author(s): Lynn Matthews (MIT Haystack Observatory)

121.05 – Soft X-ray Emission from theCentral Star of the Dumbbell NebulaThe hot central star of the well-studied planetary nebula M27 (a.k.a. Dumbbell Nebula) is a strong source of soft X-rayphotons. As part of the Chandra Planetary Nebulae Survey(ChanPlaNS), the central star was targeted with theback-illuminated (S3) chip of the Chandra ACIS-S array. Allof the central star photons detected in this observationhave photon energies below 0.3 keV, where the calibrationof Chandra is not well-constrained. Assuming the X-rayspectrum emerges from the hot photosphere, we used theX-ray spectrum and the well-known central star propertiesto constrain the relevant calibration functions (effectivearea curve and response matrix) below 0.3 keV. In thisposter, we present our methodology, results, andguidelines that will enable the use of the central star as asoft X-ray calibration source.Author(s): Rodolfo Montez (Vanderbilt University), Phillip Cargile(Vanderbilt University)

121.06 – What are the progenitors ofGalactic Bulge Planetary Nebulae?CLOUDY photoionization models of galactic bulge planetarynebulae are computed with the goal of simultaneouslydeterming the luminosity and temperature of the planetarynebulae central stars and the abundances of He, C, N, O,Ne, S, Cl, and Ar in the nebulae. A synthetic stellarevolution model is employed to determine the zero agemain sequence mass and composition of the planetarynebulae progenitor. The implications for stellar populationsand the chemical evolution of the bulge are discussed.Author(s): James Buell (Alfred State College)

121.07 – Observations Of Planetary NebulaNGC 3242 Using STIS From HST19 GO 12600During HST Cycle 19, we obtained long-slit spectra usingSTIS of the planetary nebula NGC 3242 with higher spatialresolution than previously published. The full wavelengthrange is around 1100-10200Å, covering many nebular linesfor determining numerous ionic abundances and electrondensities and temperatures. In this work, we first analyzethe low- and moderate-resolution UV emission lines ofcarbon, nitrogen and oxygen. In particular, the resolvedlines of C_III] 1907 and C_III] 1909 have yielded a directmeasurement of one of the dominant ionic species forcarbon and a determination of the density occupied bydoubly-ionized carbon and other similar ions. Next, thespatial emission profile of these lines reveals variations inthe inferred density along the line of sight from about

2800-11500 cm-3, compared with a value ~3800 cm-3,when averaged over the entire slit. Similarly, the electrontemperature is around 12000K for the entire slit and rangesfrom about 11400-14000K when the slit is divided intosmaller sub-regions. Lastly, these sub-regions of the nebulahave been modeled in detail with the photoionization codeCLOUDY. This modeling will assess the density profile thatproduces the observed density variation, reproduce thetemperature fluctuations, and constrain the central startemperature. We acknowledge the gracious support fromHST and the University of Oklahoma.Author(s): Timothy Miller (University of Oklahoma-Norman),Reginald Dufour (Rice University), Richard Henry (University of Oklahoma-Norman), Karen Kwitter (Williams College), Richard Shaw (NOAO), BruceBalick (University of Washington), Romano Corradi (IAC)

121.08 – Abundances in Eight M31Planetary NebulaeAs part of a continuing project using planetary nebulae(PNe) to study the chemical evolution and formation historyof M31 (see accompanying poster by Balick et al.), weobtained spectra of eight PNe in the fall of 2013 with theOSIRIS spectrograph on the GTC. All of these PNe arelocated outside M31’s inner disk and bulge. Spectralcoverage extended from 3700-7800Å with a resolution of~6 Å. Especially important in abundance determinations isthe detection of the weak, temperature-sensitive auroralline of [O III], at 4363Å, which is often contaminated by Hg I4358Å from streetlights; the remoteness of the GTCeliminated this difficulty. We reduced and measured thespectra using IRAF, and derived nebular diagnostics andabundances with ELSA, our in-house five-level-atomprogram. Here we report the chemical abundancesdetermined from these spectra. The bottom line is that theoxygen abundances in these PNe are all within a factor of2-3 of the solar value, (as are all the other M31 PNe ourteam has previously measured) despite the significantrange of galactocentric distance. Future work will use theseabundances to constrain models of the central star toestimate progenitor masses and ages. In particular we willuse the results to investigate the hypothesis that these PNemight represent a population related to the encounterbetween M31 and M33 ~3 Gy ago. We gratefullyacknowledge support from Williams College.Author(s): Kerry Hensley (Williams College), Karen Kwitter (WilliamsCollege), Romano Corradi (Instituto de Astrofísica de Canarias), R. Galera-Rosillo (Instituto de Astrofísica de Canarias), Bruce Balick (University ofWashington), Richard Henry (University of Oklahoma)

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121.09 – First Results from HST19 GO12600:CNO Abundances in Seven Milky WayPlanetary NebulaeIn HST Cycle 19 we observed 10 Milky Way planetarynebulae (PNe) from 1150–10270Å with STIS to obtainaccurate abundances of carbon, nitrogen and oxygen. Theultimate goal of the project is to assess carbon productionin the low-to-intermediate-mass (LIMS) progenitors of PNewith near-solar metallicity (~0.5-1.2 x solar), but varyingN/O (~0.1-3), comparing observational data withtheoretical models of carbon yields. Seven of our objectshad data of sufficient quality to allow good empiricalabundance determinations: IC2165, IC3568, NGC2440,NGC3242, NGC5315, NGC5882, and NGC7662. Each PN wasobserved with seven grating setting combinations withidentical slit positions and slit sizes across the entireUV-optical spectral region. We created one-dimensionalspectra from the two-dimensional STIS spectral images,taking care to extract the identical spatial region from eachspectrum for a given object. This was done to produceone-dimensional spectral lines integrated along the slit,resulting in the highest signal-to-noise measurements foranalysis. We measured line fluxes with IRAF and calculatednebular diagnostics and abundances with ELSA. The crucialvalue in using STIS is the ability to observe the ultravioletlines of important CNO ions with higher signal-to-noise than

in previous studies. In all objects we detected lines of C+,

C+2, and C+3. We also detected N+ and N+4 in all objects;

in four of the seven we also detected N+2 and N+3. We willpresent these data and compare them with previousdeterminations and analyses (largely from the old IUEdatasets and studies). We gratefully acknowledge supportfrom HST and from Williams College.Author(s): Karen Kwitter (Williams College), Reginald Dufour (RiceUniversity), Richard Shaw (NOAO), Richard Henry (University ofOklahoma), Bruce Balick (University of Washington), Romano Corradi (IAC)

121.10 – Kinetic Simulations of theElectrically Charged Current Sheet of aPulsarThe pulsar magnetosphere is believed to comprise avolume of low-lying, closed field about the magneticequator, bounded by polar open-field regions in which thepulsar wind flows into space. In the standard global-scalemodels, a magnetic discontinuity (electric current sheet) ofnonneutral plasma separates these opposite-polarity openfields. We use the particle-in-cell Plasma Simulation Code,PSC, to examine the dynamics of a self-consistent model forthe internal structure of this sheet, in which the charge-neutral Vlasov/Maxwell equilibria of Harris (1962) and Hoh(1966) are generalized to allow a net electric charge. PSCaccommodates both Maxwell (nonrelativistic) andJüttner/Synge (relativistic) distribution functions for theelectrons and positrons. Numerical equilibrium solutions tothe 1D Maxwell equations are initialized on the 2D PSC grid,supplemented by periodic boundary conditions in thedirection parallel to the sheet and insulating-wall boundaryconditions remote from the sheet in the perpendiculardirection. As is typical in kinetic studies of pair plasmas, theparticle thermal energy and the relative drift velocitydriving the current are assumed to be of order the restenergy and the speed of light, respectively. In this limit, theDebye length, skin depth, and Harris/Hoh current-sheetwidth are all comparable to each other, rather than widelyseparated and arranged in order of increasing size asgenerally occurs in nonrelativistic plasmas. Thequalitatively new feature of our pulsar simulations is theequilibrium electric field, whose strength can becomparable to that of the magnetic field in the relativisticlimit. We expect its presence to have profoundconsequences for the linear stability and nonlinearevolution of charged pulsar current sheets, substantiallymodifying the tearing and reconnection of the magneticfield. Exploratory PSC simulations of magnetic reconnectionin representative electrified Harris/Hoh equilibria will bepresented. The derivation, solution, and analysis of theequilibrium Vlasov/Maxwell equations are discussed in acompanion paper at this conference (C. R. DeVore et al.2014). This work was supported by NASA GSFC’s ScienceInnovation Fund.Author(s): Carrie Black (CUA), C. DeVore (NASA/GSFC), Spiro Antiochos(NASA/GSFC), Alice Harding (NASA/GSFC), Demosthenes Kazanas(NASA/GSFC), Constantinos Kalapotharakos (NASA/GSFC), Andrey Timokhin(UMD)

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121.11 – A Model for the ElectricallyCharged Current Sheet of a PulsarGlobal-scale electromagnetohydrodynamic solutions for themagnetosphere of a pulsar consist of a region of low-lying,closed magnetic field near the star bounded by opposite-polarity regions of open magnetic field along which thepulsar wind flows into space. Separating these open-fieldregions is a magnetic discontinuity – an electric currentsheet – consisting of nonneutral plasma. We havedeveloped a self-consistent model for the internal structureof this sheet by generalizing the charge-neutralVlasov/Maxwell equilibria of Harris (1962) and Hoh (1966)to allow a net electric charge. The resulting equations forthe electromagnetic field are identical for Maxwell(nonrelativistic) and Jüttner/Synge (relativistic) distributionfunctions of the particles. The solutions have a single signof net charge everywhere, with the minority populationconcentrated near the current sheet and the majoritypopulation completely dominant far from the sheet. As thefractional charge imbalance at the sheet increases, forfixed relative drift speed and total thermal pressure of theparticles, both the electric- and magnetic-field strengths farfrom the sheet increase. The electrostatic force acts todisperse the charged particles from the sheet, so themagnetic force must increase proportionately, relative tothe charge-neutral case, to pinch the sheet together andmaintain the equilibrium. The charge imbalance in thesheet that can be accommodated has an upper bound,which increases monotonically with the relative drift speed.Implications of the model for the steady-state structure ofpulsar magnetospheres will be discussed. The model alsoprovides a rigorous starting point for investigatingelectromagnetohydrodynamic and kinetic instabilities thatcould lead to magnetic reconnection and current-sheetdisruption in pulsars. Exploratory particle-in-cell simulationsof representative equilibria are presented in a companionpaper at this conference (C. E. Black et al. 2014). This workwas supported by NASA GSFC’s Science Innovation Fund.Author(s): C. DeVore (NASA GSFC), Spiro Antiochos (NASA GSFC),Carrie Black (NASA GSFC), Alice Harding (NASA GSFC), ConstantinosKalapotharakos (NASA GSFC), Demosthenes Kazanas (NASA GSFC), AndreyTimokhin (NASA GSFC)

121.12 – X-Ray Observations of TwoRemarkable Millisecond Pulsars: PSRJ0337+1715 and PSR J0636+5129PSR J0337+1715 is a fast, bright, and so-far uniquemillisecond pulsar (MSP) in a hierarchical triple system withtwo white dwarf (WD) companions. PSR J0636+5129 is anMSP in a 96-min orbit with a companion with a mass ofapprox. 8 M,J,. Here we report recent observations of thesesystems with the XMM-Newton X-ray telescope. We haveanalyzed X-ray spectroscopy and optical/ultravioletphotometry. The X-ray data for each seem largelyconsistent with expectations for most MSPs. Theoptical/ultraviolet data help us determine the extinctionand size of the inner WD companion to J0337 as well as theeffects of the outer, more massive WD. We discuss theimplications of these data and prospects for the future.Author(s): Renée Spiewak (University of WI - Milwaukee), DavidKaplan (University of WI - Milwaukee), Kevin Stovall (University of NewMexico), Duncan Lorimer (West Virginia University), Maura McLaughlin(West Virginia University), Ingrid Stairs (University of British Columbia),Ryan Lynch (McGill University), Scott Ransom (NRAO), Jason Hessels(ASTRON), Anne Archibald (ASTRON)

Contributing teams: The GBT Driftscan Collaboration

121.13 – Host Galaxy Environments ofSuperluminous SupernovaeOne of the most unexpected results from Pan-STARRS andother untargeted time-domain surveys is the discovery ofsuper-luminous supernovae (SLSNe), with bolometricluminosities up to 100 times that of normal core-collapse,Type Ia SNe, and even GRB-SNe and with spectra that donot match any known SN classes. These SLSNe represent anew challenge to our understanding of the death ofmassive stars, the standard core-collapse picture, and themechanism for powering optical emission in SNe. Progressin our understanding will come from both studying theproperties of the SNe themselves, as well as studying theirgalactic and sub-galactic environments. We will presentresults from an extensive survey of ~30 SLSN hostgalaxies, spanning a redshift range of 0.1 < z < 1.6. Ourdata includes optical and NIR photometry and opticalspectroscopy, allowing us to determine stellar masses, starformation rates and metallicities, as well as HST imagingallowing us to study the host morphologies and thelocations of the SLSNe in the overall host light distribution.We will compare the SLSN host properties to core-collapseSN host galaxies and long-duration GRB host galaxies in thesame redshift range, shedding light on the possibleprogenitors of these extreme explosions.Author(s): Ragnhild Lunnan (Harvard University), Ryan Chornock(Harvard University), Edo Berger (Harvard University)

Contributing teams: Pan-STARRS1 CfA Transients Group

121.14 – Using PNe to Explore the History ofM31's Extended DiskThe results of O/H abundances derived from PNe in M31(accompanying poster by Hensley et al.) have extended theradius coverage of our previous gradient studies out toprojected disk distances of 100 kpc. The PNe are drawnfrom the peak of the [OIII] PNLF which suggests that theirprogenitor stars are more massive than about 1.5 M_sunwith evolution lifetimes less than ~2 billion years. However,many of the PNe in this sample are located in regionswithout gas and other signatures of recent star formation.Here we investigate how the measured O/H abundances ofPNe beyond the classical disk of M31 correlate within stellargroupings that are defined in various ways (region, diskradius, kinematic deviations from a thin disk model, andproximity to known stellar streams). The goal is todetermine the relationships of the M31 PN sample to any HIand the other stellar populations associated with theevolution of M31's outer environment.Author(s): Bruce Balick (Univ. of Washington), Karen Kwitter(Williams College), Romano Corradi (IAC), Kerry Hensley (Williams College),Richard Henry (Univ. of Oklahoma)

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121.15 – SweetSpot Data Release 1: 70 TypeIa Supernovae in the Near Infrared in theNearby Hubble FlowSweetSpot is an NOAO Survey program from 2012B-2015Athat is observing 150 Type Ia supernovae (SNe Ia) in theHubble flow to obtain reliable NIR luminosities free frompeculiar-velocity confusion and the uncertainties of dust.Our full SweetSpot program will (1) extend the NIR Hubblediagram past currently available samples; (2) quantitativelydemonstrate the degree to which SNeIa are robust standardcandles in the NIR; (3) provide key insights about the colorevolution and intrinsic properties of SNeIa and their hostgalaxies; and (4) establish a well-calibrated low-redshiftanchor for future NIR supernova surveys from JWST, Euclid,and WFIRST/NEW. By the end of the survey we will havemeasured the relative distance to a redshift of z~0.05 to1%. Nearby Type Ia supernova (SN Ia) observations such asthese will test the standard nature of SNe Ia in therestframe NIR, allow insight into the nature of dust, andprovide a critical anchor for future cosmological SN Iasurveys at higher redshift. We here present a first look atour Data Release 1 which includes 70 supernovae observedfrom 2012B-2013B.Author(s): W. Wood-Vasey (University of Pittsburgh), Anja Weyant(University of Pittsburgh), Lori Allen (NOAO), Peter Garnavich (NotreDame), Nabila Jahan (University of Pittsburgh), Saurabh Jha (RutgersUniversity), Kara Ponder (University of Pittsburgh), Richard Joyce (NOAO),Thomas Matheson (NOAO), Armin Rest (STScI)

121.16 – The Supernova SpectropolarimetryProject: Photometric Followup in the Opticaland Near-Infrared by the Mount LagunaSupernova SurveyThe SuperNova SpectroPOLarimetry project (SNSPOL) is arecently formed collaboration between observers andtheorists that focuses on decoding the complex,time-dependent spectropolarimetric behavior ofsupernovae (SNe) of all types. Photometric followup oftargeted SNe is provided by the MOunt LAguna SUpernovaSurvey (MOLASUS), which is carried out using MountLaguna Observatory's 1-meter telescope. Here we presentoptical and near-infrared (NIR) photometric observations ofthree recent SNe that were observed as part of thiscoordinated effort: SN 2013ej, SN 2013dy, and SN 2014J.We discuss the multi-band light curves of these three SNe,with a particular focus on the use of NIRIM (Meixner et al.1999), our NIR camera used to obtain the J, H, and K' data.SN 2013ej is a Type II supernova in M74, discovered by theLick Observatory Supernova Search (LOSS) on 2013 July25.45 (UT; UT dates are used throughout). Our monitoringof this object began 2013 August 07.88 and continued until2013 December 13.74. The data provide evidence for aphotospheric phase lasting roughly 70 days from our firstobservation, with SN 2013ej then declining by about 3magnitudes in H-band over the following 50 days. SN2013dy is a Type Ia supernova in NGC 7250 discovered byLOSS on 2013 July 10.45. We monitored SN 2013dy fromJuly 19.89 until 2013 December 13.62. Our observationsshow a characteristic type Ia light curve that declines inbrightness by about 3 magnitudes in H through the courseof our monitoring. Lastly, SN 2014J is a Type Ia-HV [HighVelocity] (Takaki et. al (2014) - ATEL 5791) in M82,discovered on 2014 January 21.81, and the closest Type Iasupernovae in over three decades. Our monitoring of SN2014J began on 2014 January 30.67. We acknowledgesupport from NSF grants AST-1009571 and AST-1210311,under which part of this research was carried out.Author(s): Harish Khandrika (San Diego State University), DouglasLeonard (San Diego State University), Chuck Horst (San Diego StateUniversity), Alisa Rachubo (San Diego State University), Nhieu Duong (SanDiego State University), G. Grant Williams (MMT Observatory), Paul Smith(Steward Observatory), Nathan Smith (Steward Observatory), Peter Milne(Steward Observatory), Jennifer Hoffman (U. Denver), Leah Huk (U.Denver), Luc Dessart (Universite de Nice)

121.17 – SN 2014J and the HarvardObserving ProjectA chance discovery on January 21, 2014 by Steve Fossey etal. of University College London during an undergraduatetelescope training session revealed the closest type Iasupernova in the past 42 years. The bright SN 2014J wasobserved by undergraduates and graduate students alike inthe Harvard Observing Project (see poster by A. Bieryla)with the Clay Telescope at Harvard University. Observationswere obtained in multiple filters starting January 24, 2014,prior to the supernova reaching its peak brightness, andmonitoring will continue as the supernova fades inbrightness. We will present multiple band light curvephotometry and color RGB images of SN 2014J and its hostgalaxy M82.Author(s): Melissa McIntosh (Harvard University), Allyson Bieryla(Harvard University), Elisabeth Newton (Harvard University), John Lewis(Harvard University), Andrew Vanderburg (Harvard University), KateAlexander (Harvard University), Peter Blanchard (Harvard University)

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121.18 – SN 1993J - The X-ray Story of aSupernova Slowly Transitioning to aRemnantSupernova 1993J in the nearby galaxy M81 is one of thebest observed supernovae (SNe) in X-rays, with betterlong-term X-ray time-sampling than any other SN. Were-analysed most of the available archival data on SN1993J, combined with a 79ks Chandra observation obtainedby our group in Aug 2010. Together, the data constitute averitable history of a Type IIb SN from its explosion, throughits outward journey into the surrounding medium, and onits way to becoming a remnant. The X-ray emission probesthe characteristics of the surrounding medium, and thekinematics of the SN shock wave(s). In this project weexplore the evolution of these quantities in SN 1993J,together with the evolution of its X-ray spectrum.Author(s): Vikram Dwarkadas (Univ. of Chicago), Franz Bauer (SpaceScience Institute)

121.19 – The Curious Case of SN 2011dn:Was It A Peculiar Type Ia Supernova?Type Ia supernovae (SNe Ia) are excellent cosmologicaldistance indicators due to the uniformity in their lightcurves. This led to the major discovery of the acceleratedexpansion of the universe (Riess et al. 1998, Perlmutter etal. 1999). However, SNe Ia are not so uniform as one mayexpect, as there are many ‘peculiar’ SNe Ia that exhibitdifferences in photometry and spectroscopy from normalSNe Ia. One of the goals of supernova cosmology today isto produce a cleaner sample of SNe Ia by removing thepeculiar SNe Ia from the sample. A useful parameter foridentifying peculiar SNe Ia based on photometry is?m15(B), which measures the decrease in B-bandmagnitude 15 days after the peak of the light curve (Phillipset al. 1993). For typical SNe Ia the standard value is?m15(B) = 1.1. Peculiar SNe Ia of the overluminous typeshow a slower decline, with its prototypical member SN1991T having ?m15(B) = 0.80 (Hicken et al. 2009), whilepeculiar SNe Ia of the subluminous type show a fasterdecline, with its prototypical member SN 1991bg having?m15(B) = 1.87 (Hicken et al. 2009). Here we presentoptical photometry and spectroscopy of SN 2011dn, whichwere obtained as part of the MOunt LAguna SUpernovaSurvey (MOLASUS). Based on its pre-maximum spectrum,which showed strong absorption lines of Fe III ?4404 and FeIII ?5129, along with a weak Si II ?6355 absorption line, SN2011dn was classified as a SN 1991T-like event (Koff et al.2011). However, in an earlier preliminary analysis of thelight curves – based on point-spread-function photometry –we proposed that SN 2011dn might have had a higher thanexpected ?m15(B) value of 1.08 (Salvo et al. 2012). SinceSN 2011dn is embedded in its host galaxy UGC 11501, it ispossible that some of the light from the host galaxy wasmeasured, which may have influenced the measured?m15(B) value. Here, we employ galaxy-subtractiontechniques to isolate the supernova light from its hostgalaxy, and generate more precise light curves. We derivean updated value of ?m15(B), in order to verify or refutethe claimed peculiarity of SN 2011dn. We acknowledgesupport from NSF grants AST-0850564, AST-1009571 andAST-1210311, under which part of this research was carriedout.Author(s): Alisa Rachubo (San Diego State University), Chris Salvo(University of California, Riverside), Douglas Leonard (San Diego StateUniversity), Nhieu Duong (San Diego State University), Chuck Horst (SanDiego State University), Harish Khandrika (San Diego State University),Julienne Sumandal (San Diego State University), John Moustakas (SienaCollege)

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121.20 – Photometry of the Supernova SN2011dh in the Whirlpool GalaxySupernovae are categorized by the presence (Type II) orabsence (Type I) of hydrogen lines in their spectra. Ourobject of interest, SN 2011dh is categorized by its earlyhydrogen lines and dominated by helium lines in the laterphases, indicating a type IIb supernova (Ergon et al. 2013).Here, we present optical photometry of the SN 2011dh,which was obtained as part of the MOunt LAgunaSUpernova Survey (MOLASUS) over a period of almost twoyears capturing the entire lifespan in four different filters(BVRI). All photometric measurements were made usingIRAF, and employing point-spread-function fittingtechnique. We discuss and analyze the light curvesproduced. We acknowledge support from NSF grantsAST-0850564, AST-1009571 and AST-1210311, under whichpart of this research was carried out.Author(s): Nhieu Duong (San Diego State University), JulienneSumandal (San Diego State University), Douglas Leonard (San Diego StateUniversity), Alisa Rachubo (San Diego State University), Harish Khandrika(San Diego State University), Chris Salvo (university of california riverside),Chuck Horst (San Diego State University)

121.21 – Evidence for AcceleratedRadioactive Decay (ARD) Models of Type ISupernova Lightcurves in the Low RedshiftUniverseForty years ago Van Hise [ApJ 192 (1974) 657-659]observed that the post peak light curve for the Type Isupernova SN1937C is well represented by a sum of twoexponentials with half lives which are ~ 0.75 of the

terrestrial half lives of 56Ni and 56Co in the beta decay

chain 56Ni ? 56Co ? 56Fe. Thirty nine years ago Leventhaland McCall [Nature 255 (1975) 690-692] proposed a fullyconvective, radioactive white dwarf model to account forthe observed accelerated decay. Thirty eight years ago ARDmodels were tested by Rust, et al. [Nature 262 (1976)118-120] on the data from the 15 fragmentary light curvesavailable at that time. The results offered significant butnot overwhelming support for ARD models. In this paper wepresent a new mathematical model for Type I lightcurvesand fit that model, using only 6 free parameters, to anextensive collection of higher quality lightcurves that havebeen measured over the last 38 years. The fits all capturemore than 99% of the total variance in the measured data,thus establishing the reality of an ARD lightcurve model.These new results provide a much improved Phillips relationfor calibrating the extragalactic distance scale and testingother cosmological relations.Author(s): Bert Rust (NIST), Marvin Leventhal (University of Maryland)

121.22 – Numerical Verification of the Whiteand Long SNR ModelIn 1991 White and Long derived a similarity solution thatdescribed the evolution of supernova remnants expandinginto an interstellar medium uniformly populated by denseclouds. While this solution marked a great advance inmodeling the IR, optical, and X-ray emissions of supernovaremnants, it was constrained by a set of limitingassumptions; namely, a homogeneous and uniforminter-cloud medium, clouds that are uniformly distributedand much denser than the surround inter-cloud medium,and no significant acceleration or heating of the clouds bythe shock. While many of these assumptions arereasonable, they limit the range of simulations to a subsetof all possible supernova remnant scenarios. In this workwe have devised a numerical simulation of a supernovaremnant expanding into an interstellar medium using theFLASH MHD code. We first test a simulation with conditionssimilar to that of the White and Long model to test thevalidity of the simulation. We then vary parameters of theclouds, such as the distribution and density ratios withrespect to the inter-cloud medium, to determine whichparameters play an important role in SNR observationalsignatures.Author(s): Henry Winter (SAO), Randall Smith (SAO), Adam Foster(SAO)

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122 – Instrumentation PostersPoster Session – Essex Ballroom and America Foyer – 02 Jun 2014 09:00 AM to 06:30 PM

122.01 – Twelve Years of the HST AdvancedCamera for Surveys : Calibration UpdateThe Advanced Camera for Surveys (ACS) has been aworkhorse HST imager for over twelve years, subsequent toits Servicing Mission 3B installation. The once defunct ACSWide Field Channel (WFC) has now been operating longersince its Servicing Mission 4 repair than it had originallyoperated prior to its 2007 failure. Despite the accumulatingradiation damage to the WFC CCDs during their long stay inlow Earth orbit, ACS continues to be heavily exploited bythe HST community as both a prime and a parallel detector.Conspicuous examples include the recently completed HSTMulti-cycle Treasury programs, and the ongoing HSTFrontier Fields (HFF) program. We review recentdevelopments in ACS calibration that enable the continuedhigh performance of this instrument, with particularattention the to the Wide Field Channel. Highlights include:1) the refinement of the WFC geometric distortion solutionand its time dependency; 2) the efficacy of bothpixel-based and catalog-based corrections for theworsening WFC charge-transfer efficiency (CTE); 3) theextension of pixel-based CTE correction to the WFC 2Ksubarray mode; and 4) a novel "self-calibration" techniqueappropriate for large-number stacks of deep WFCexposures (such as the HFF targets) that provides superiorreductions compared to the standard CALACS reductionpipeline.Author(s): Norman Grogin (Space Telescope Science Institute)

Contributing teams: the ACS Calibration Team

122.02 – Revised ACS/WFC GeometricDistortion and Its Linear Time DependencyWe present a new geometric distortion model and its timedependency for the Wide Field Channel (WFC) of the HSTAdvanced Camera for Surveys (ACS). The primary goal ofthis study is to derive a new Instrument DistortionCorrection (IDC) table to provide calibration reference filesfor superior alignment and combination of WFC images.These new calibration files will allow the STSDAS andDRIZZLEPAC software to properly align and combine ACSimages as well as cross-combine them with other HSTimages with very high accuracy. The calibrationobservations of globular cluster 47Tuc taken through theACS/WFC F435W, F606W and F814W filters before and afterServicing Mission 4 over a wide range of telescope rollangles have been used for astrometric calibration withaccuracy to the level of 0.1 pixels. From these observations,a 5th order polynomial fit was derived with respect to thestandard astrometric catalog in the vicinity of 47Tuc. Aftertransforming the filter-specific distortion polynomials intothe HST focal-plane coordinate system (V2V3), we found ahighly significant, filter independent, linear trend in thecoefficients over the lifetime of the WFC. AstroDrizzle itselfhas been slightly modified to handle properly thetime-dependency. Our extensive testing suggests that WFCgeometric distortions are now corrected to a level of <=0.1pixels across the entire field of view.Author(s): David Borncamp (Space Telescope Science Institute),Vera Kozhurina-Platais (Space Telescope Science Institute), Warren Hack(Space Telescope Science Institute), Colin Cox (Space Telescope ScienceInstitute)

122.03 – WFC3: Improvements to WFC3UVIS Photometric CalibrationThe Wide Field Camera 3 (WFC3) is a fourth-generationimaging instrument installed on the Hubble SpaceTelescope (HST) in May 2009. It contains both an IR and aUVIS channel. The latter, which covers the 200-1000nmspectral range, consists of two 2K x 4K CCD chips alongwith 62 spectral elements and one grism. The two CCDchips were manufactured on different wafers. As a result,there are differences in the two chips’ properties andbehaviors, such as their lithography imprint patterns, theirsensitivity responses, and their measured quantumefficiency (QE), particularly in the UV. Therefore, the WFC3team developed a chip-dependent approach to thephotometric calibration, where each chip now has its ownseparate calibration. We discuss the impacts of this newapproach and its implementation in the calibration pipeline,presenting the new zero points and header keywords, aswell as the new flat fields. We also present the latest trendsin the contamination monitoring, which obtains regularimaging and grism spectroscopy of the white dwarf,GRW+70, in key filters F218W, F225W, F336W, F814W, andF606W. No contamination effects have been detected,though there is evidence for a small photometric drift (<1%over 3 years). We anticipate that these efforts will improveUV imaging with WFC3.Author(s): Catherine Gosmeyer (Space Telescope ScienceInstitute), Sylvia Baggett (Space Telescope Science Institute), ArielBowers (Space Telescope Science Institute), Tomas Dahlen (SpaceTelescope Science Institute), Susana Deustua (Space Telescope ScienceInstitute), Derek Hammer (Space Telescope Science Institute), JenniferMack (Space Telescope Science Institute)

122.04 – WFC3: UVIS Dark CalibrationWide Field Camera 3 (WFC3), a fourth-generation imaginginstrument on board the Hubble Space Telescope (HST), hasexhibited excellent performance since its installation duringServicing Mission 4 in May 2009. The UVIS detector,comprised of two e2v CCDs, is one of two channelsavailable on WFC3 and is named for its ultraviolet andvisible light sensitivity. We present the various proceduresand results of the WFC3/UVIS dark calibration, whichmonitors the health and stability of the UVIS detector,provides characterization of hot pixels and dark current,and produces calibration files to be used as a correction fordark current in science images. We describe the long-termgrowth of hot pixels and the impacts that UVIS ChargeTransfer Efficiency (CTE) losses, postflashing, and proximityto the readout amplifiers have on the population. We alsodiscuss the evolution of the median dark current, which hasbeen slowly increasing since the start of the mission and iscurrently ~6 e-/hr/pix, averaged across each chip. Weoutline the current algorithm for creating UVIS darkcalibration files, which includes aggressive cosmic raymasking, image combination, and hot pixel flagging.Calibration products are available to the user community,typically 3-5 days after initial processing, through theCalibration Database System (CDBS). Finally, we discussvarious improvements to the calibration and monitoringprocedures. UVIS dark monitoring will continue throughoutand beyond HST’s current proposal cycle.Author(s): Matthew Bourque (STScI), John Biretta (STScI), JayAnderson (STScI), Sylvia Baggett (STScI), Heather Gunning (STScI), JohnMacKenty (STScI)

Contributing teams: The WFC3 Team

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122.05 – WFC3/UVIS Charge-Transfer-Efficiency Losses: Mitigation and CorrectionWFC3/UVIS was installed on HST in 2009 and has beensubjected to the harsh radiation environment of space forthe past five years. One consequence of radiation damageis charge-transfer-efficiency (CTE) losses, and these lossesbecame apparent much more quickly than expected forWFC3/UVIS because of its low dark current and the lowbackgrounds in the ultraviolet. Several years ago, wedeveloped a pixel-based model to describe the WFC3/UVIScharge-transfer process, similar to the model that wasdeveloped for ACS/WFC. This model showed us that alow-level of post-flash (12 electrons) significantly improvesCTE, and many observations now take advantage of thispreventative strategy. We have recently taken somecalibration data to allow us to improve the pixel-basedCTE-correction model in anticipation for the model'sinclusion in the WFC3 pipeline. This poster will report on thelatest model and CTE-losses.Author(s): Jay Anderson (STScI)

Contributing teams: WFC3 Team

122.06 – WFC3: News Regarding IRBackgrounds, Spatial Scans, and Cycle 22Phase 2 AdviceWe report on recent developments in the characterizationand calibration of the Hubble Space Telescope's Wide FieldCamera 3. Installed in 2009 during HST Servicing Mission 4,WFC3 continues as the most used instrument on theobservatory with stable performance and steadyimprovements in its photometric, flat field, dark current,and astrometric calibrations. An important recentdevelopment is the recognition of the impact of the Helium1.083 micron emission line from the upper atmosphere.This sometimes results in significant background variationsof factors of 3 to 5 higher than the nominal zodiacal lightbackground in the F105W, F110W, G102, and G141 spectralelements. We also report on progress in using observatorylevel spatial scans to achieve higher dynamic rangeobservations, to obtain higher precision and more efficientphotometric measurements of bright sources, to improveour knowledge of the flat fields, and to increase theprecision of astrometric measurements. Suggestions to aidCycle 22 Phase 2 proposers will also be presented.Author(s): John MacKenty (STScI)

Contributing teams: Wide Field Camera 3

122.07 – Advanced Time-domainCalibrations and Data-reductionTechniqueswith HST/COS.The Hubble Space Telescope/Cosmic Origins Spectrograph(HST/COS) detectors have a time-tag mode of observationin which the arrival time of each photon is recordedindividually. Although the COS calibration pipeline (CalCOS)makes use of this capability in many aspects of routineprocessing, there remains a number other ways that thisinformation can be used to improve the calibration forspecific science cases. This has led to the development oftools and techniques to perform additional calibrations thatare not part of the standard data products output byCalCOS, but have been made available to the user. Here wedemonstrate a few of these techniques including day/nightfiltering, extracting spectra on sub-exposure timescales,producing photometric light-curves, and performingadditional dark-count screening.Author(s): Justin Ely (Space Telescope Science Institute), K.Bostroem (Space Telescope Science Institute), John Debes (EuropeanSpace Agency), Svea Hernandez (Space Telescope Science Institute), PhilipHodge (Space Telescope Science Institute), Robert Jedrzejewski (SpaceTelescope Science Institute), Kevin Lindsay (Space Telescope ScienceInstitute), Derck Massa (Space Science Institute), Cristina Oliveira(European Space Agency), Steven Penton (Space Telescope ScienceInstitute), Charles Proffitt (Space Telescope Science Institute), JuliaRoman-Duval (European Space Agency), David Sahnow (Space TelescopeScience Institute), Hugues Sana (European Space Agency), PauleSonnentrucker (European Space Agency), Joanna Taylor (Space TelescopeScience Institute)

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122.08 – Moving COS FUV Spectra to theThird COS FUV Lifetime PositionIn the fall of 2014, the location of COS FUV spectra on thedetector is expected to be moved from the second COS FUVLifetime Position (LP2) to the third COS FUV LifetimePosition (LP3). This move is needed to mitigate thecontinuing effects of gain sag in the microchannel platedetectors. With the LP2 move (July 2012) spectra wereshifted perpendicularly to the dispersion direction by theequivalent of +3.5", or about 41 pixels, from the originalLP1 location. With the LP3 move, spectra will be shiftedbelow the original LP1 position by about -2.5", whichmaximizes resolution and the detector area available forfuture lifetime positions. The modes with the widest profilesperpendicular to the dispersion, G130M 1055 and 1096, willremain at LP2, while all other modes will be moved to LP3.Improved extraction techniques are being developed toensure that the gain sagged regions near LP1 do not affectthe spectral quality of point source observations at LP3. Wewill present results from preliminary tests near LP3 anddiscuss the implications for science observations. Typicalspectral resolving power (?/??) for the modes that aremoved to LP3 may decline by about 15% relative to theperformance at LP2. Observations of spatially extendedsources may also be slightly impacted by the proximity tothe gain sagged regions near the original LP1 location andcare may be needed not to confuse gain sag artifacts withreal spectral features for such sources. Instrumentperformance is otherwise expected to be similar to thatseen during Cycle 21.Author(s): Charles Proffitt (Space Telescope Science Institute), K.Bostroem (Space Telescope Science Institute), John Debes (EuropeanSpace Agency), Justin Ely (Space Telescope Science Institute), SveaHernandez (Space Telescope Science Institute), Philip Hodge (SpaceTelescope Science Institute), Robert Jedrzejewski (Space Telescope ScienceInstitute), Kevin Lindsay (Space Telescope Science Institute), Derck Massa(Space Science Institute), Cristina Oliveira (European Space Agency),Steven Penton (Space Telescope Science Institute), Julia Roman-Duval(European Space Agency), David Sahnow (Space Telescope ScienceInstitute), Hugues Sana (European Space Agency), Paul Sonnentrucker(European Space Agency), Joanna Taylor (Space Telescope ScienceInstitute)

122.09 – Planetary Imaging ConceptTestbed Using a Recoverable Experiment -CoronagraphWe present the design and expected performance ofPICTURE-C, a new suborbital mission designed to imagedebris disks around stars hosting exoplanets. We presentthe mission design, expected capabilities, and status.Potential targets, observing scenarios, and expected resultsare also discussed.Author(s): Timothy Cook (UMass Lowell), Kerri Cahoy (MIT), NikoleLewis (MIT), Mark Swain (JPL), Susanna Finn (UMass Lowell), ChristopherMendillo (UMass Lowell), Supriya Chakrabarti (UMass Lowell), Jason Martel(UMass Lowell), Ewan Douglas (Boston University)

122.10 – Status of the PICTURE SoundingRocket to Image the Epsilon EridaniCircumstellar EnvironmentThe PICTURE (Planetary Imaging Concept Testbed Using aRocket Experiment) sounding rocket will use a visiblenulling interferometer to characterize the exozodiacal dustdisk of Epsilon Eridani (K2V, 3.22 pc) in reflected visiblelight to an inner radius of 1.5 AU (0.5”) from the star.Launch is scheduled for Fall 2014 and the PICTURE payloadis currently undergoing re-integration. The first launch ofPICTURE suffered a science telemetry failure and theprimary mirror was shattered upon landing, the secondlaunch will fly a new SiC primary mirror and onboard datastorage. PICTURE visible light observations will constrainscattering properties of the Epsilon Eridani exozodiacal dustdisk from 600nm to 750 nm, measuring the backgroundbrightness which must be overcome for future exoplanetobservations. Additionally, PICTURE will demonstrateoperation of a MEMS deformable mirror and a visible nullingcoronagraph in space. We will present the latestmeasurements of integrated telescope and interferometerperformance.Author(s): Ewan Douglas (Boston University), Christopher Mendillo(University of Massachusetts Lowell), Brian Hicks (NASA GSFC), TimothyCook (University of Massachusetts Lowell), Jason Martel (University ofMassachusetts Lowell), Susanna Finn (University of Massachusetts Lowell),Ronald Polidan (Northrop Grumman Aerospace Systems), SupriyaChakrabarti (University of Massachusetts Lowell)

122.11 – High Precision Pointing Stabilityand Control for Exoplanet MissionsExoplanet imaging and characterization spaceobservatories require high precision pointing stability andstability. We have developed a toolbox of sensors, actuatorsand algorithms along with a systems approach to meet thedemanding needs of these missions. Grown fromdevelopments and experience gained from high precisionEarth remote sensing missions such as the WorldViewsatellites, as well as high performance astrophysicsmissions such as Kepler and JWST, these capabilities areenabling for a wide range of future missions. Theapproaches take advantage of highly flexible softwarearchitectures; Enhanced ground simulation capabilities forsystem tuning and verification and validation; Testingcapabilities to verify our modelling; High precision sensorsincluding sub-arc-second star trackers and fine guidancesensors; High bandwidth fast steering mirrors for opticalpath control; and high precision reaction wheels and controlmoment gyros for overall observatory control. Many ofthese capabilities coupled with innovative thinking havebeen applied to the recent Kepler mission to enable the K2extended mission concept.Author(s): Arnold Barnes (Ball Aerospace), John Troeltzsch (BallAerospace), Doug Wiemer (Ball Aerospace)

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122.12 – Modeling Exoplanet TransmissionSpectra with Solar System ObjectsLight transmitted through the atmosphere of an extrasolarplanet during a transit becomes encoded with informationabout the composition and structure of the exoplanet’satmosphere. Transit transmission spectroscopy aims toextract this information through observations of theexoplanet’s wavelength-dependent transit depth. However,this practice often yields results with degenerateinterpretations. For instance, a featureless transmissioncurve could suggest an atmosphere with a large meanmolecular weight, high-altitude clouds, or it could simplysuggest that the instruments making the measurementsare not sensitive enough to detect any subtle spectralfeatures. As the number of known exoplanets continues togrow, so does the importance of our ability to accuratelycharacterize these exoplanets using methods such astransit transmission spectroscopy. Fortunately, the bodiesin our own solar system can serve as laboratories tounderstand extrasolar planetary systems. We present amodel that can transform solar occultation data intotransmission spectra of the atmospheres of various bodieswithin our solar system. Using this model, we can improveour current interpretations of exoplanetary transmissionspectra through observations well-studied solar systemobjects, as if they were exoplanets. The transformationfrom occultation to transit presents several challengesincluding those due to refraction, viewing geometry, andlimb darkening. However, we show that it is possible toextract a wavelength-dependent, star-planet radius ratioand therefore a transmission spectrum from occultationdata. This model is originally intended for use on Saturnand Titan utilizing occultations observed by the Visual andInfrared Mapping Spectrometer (VIMS) onboard the CassiniSpacecraft. However, it has the potential to be applied toother planets and satellites, even those exhibiting thinatmospheres such as Mars. As future missions such as TESSand JWST continue to emphasize the importance ofexoplanet characterization, it is critical that we understandthe potential of transit transmission spectroscopy.Author(s): Paul Dalba (Boston University), Philip Muirhead (BostonUniversity), Matthew Hedman (University of Idaho), Jonathan Fortney(University of California, Santa Cruz), Philip Nicholson (Cornell University)

122.13 – The Effects of Orbital Environmenton X-ray CCD PerformanceX-ray telescopes, such as NASA's Chandra X-rayObservatory and Japan's Suzaku, have flown in space forseveral decades, however the effects of this hostileenvironment on sensitive astrophysics instruments are stillnot completely documented. Both observatories use CCDcameras for imaging spectroscopy of the X-ray sky. TheCCDs themselves are similar in design, being fabricated atMIT's Lincoln Laboratory. We compare the on-orbitperformance evolution of the Chandra ACIS and Suzaku XIS,to better understand the effect of the radiationenvironment in low- and high-Earth orbit. After more than acombined twenty years in space, both instruments havesuffered performance degradation due to radiationdamage, but comparison must take into consideration theoperational differences, such as the presence of chargeinjection and the warmer focal plane temperature of theXIS. The low-Earth orbit of Suzaku has the advantage of alower and stable particle background during observations,while the Chandra particle background during observationsis higher and subject to variations due to the solar cycleand solar storms. This is in contrast to the rate of radiationdamage accumulation, which is about four times higher forSuzaku, even after correcting for operational differences.We present models of the particle environments for bothSuzaku and Chandra which can explain the apparentdiscrepancy. While the choice of orbit for future missions isobviously dependent on many factors beyond radiationenvironment, we hope this study will be useful for betterinforming that choice.Author(s): Catherine Grant (MIT), Beverly LaMarr (MIT), Eric Miller(MIT), Mark Bautz (MIT)

122.14 – An X-ray Grating Spectrometer forthe ISSWe present the design approach for a X-ray gratingspectrometer mission to be deployed on the InternationalSpace Station. The baseline design uses sub-aperturedX-ray optics feeding into off-plane gratings to achieve bothhigh spectral resolution with a large effective area; the readout is by high-TRL CCDs in the focal plane. The mission willuse a pointing system with a novel technology to reducevibrations from the ISS propagating into the telescope, andwould be ready to be attached to the ISS in 2021. Themission parameters are similar to those of the IXO X-rayGrating Spectrometer of R=3000 and ~1000 sq. cm at 0.5keV, with a bandpass from ~0.3-1 keV, enabling a widerange of science objectives.Author(s): Jay Bookbinder (Smithsonian Astrophysical Obs.),Randall McEntaffer (U. Iowa), Peter Daigneau (Smithsonian AstrophysicalObs.), Randall Smith (Smithsonian Astrophysical Obs.), Mark Bautz (MIT),David Burrows (Penn State ), Richard Willingale (Univ. of Leicester), RobertPetre (GSFC), Jörn Wilms (Friedrich-Alexander Universitaet), AbrahamFalcone (Penn State ), Nancy Brickhouse (Smithsonian Astrophysical Obs.),Andrew Ptak (GSFC), Adam Foster (Smithsonian Astrophysical Obs.), JoelBregman (U. Michigan)

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122.15 – Micro-X X-ray ImagingSpectrometerMicro-X is a NASA funded, rocket borne X-ray imagingspectrometer utilizing Transition Edge Sensors (TESs) toperform high resolution microcalorimetry in the soft X-rayband on astronomical sources. The TESs utilize the 50 mKstage of an Adiabatic Demagnetization Refrigerator (ADR)as a heat sink – one of the biggest challenges in payloaddesign and calibration is to maintain the temperature of thedetectors. To achieve the best thermal environment andtherefore the best possible resolution of the detectors, wecombine software modeling of heat flow within theinstrument with data from laboratory tests of thermalconnections between the Front End Assembly and ADR. Wepresent a brief overview of the instrument design, recentlab results and modeling, and an update of ongoingprogress with the preparations for launch.Author(s): David Goldfinger (Massachusetts Institute ofTechnology)

Contributing teams: Micro-X Collaboration

122.16 – From ProtoEXIST to HREXIThe ProtoEXIST program was initiated for the creation of ahighly scalable, cost effective, CdZnTe (CZT) detector planearchitecture. Two separate prototype coded-aperturetelescopes, (ProtoEXIST1 and ProtoEXIST2) each with adetector plane consisting of an 8 × 8 array of pixelated 2cm × 2 cm, 5 mm thick CZT detectors with anode pixelpitches of 2.5 mm (P1) and 0.6048 mm (P2) and a focallength of ~900 mm have been successfully integrated andflown on high-altitude (39 km) balloon flights in 2009 and2012 demonstrating operation in space-like conditionswhile conducting observations of X-ray sources. We reviewthe performance of the P1 and P2 detectors and telescopesbefore, during and after flight and discuss forthcomingupgrades to the detector plane architecture. We thendescribe our follow-on High Resolution Energetic X-rayImager (HREXI) program intended for eventual deployment

as a large area (>1m2) low cost coded-aperture telescopeto conduct a wide-field hard X-ray imaging survey andtransient monitor optimize over 3-200 keV band. Withsensitivities and resolution (both spatial and spectral)~5-10X better than Swift/BAT, HREXI will be proposed for afuture Explorer class mission.Author(s): Branden Allen (Harvard-Smithsonian CfA), JaeSub Hong(Harvard-Smithsonian CfA), Jonathan Grindlay (Harvard-Smithsonian CfA),Scott Barthelmy (Goddard Space Flight Center), Robert Baker (GoddardSpace Flight Center), Peter Mao (Caltech), Fiona Harrison (Caltech),Hiromasa Miyasaka (Caltech), Jill Burnham (Caltech), William Cook(Caltech)

122.17 – Optical All-Sky Camera for theLarge Synoptic Survey TelescopeThe Large Synoptic Survey Telescope (LSST) is a wide-field8.4 meter telescope that will repeatedly survey thesouthern sky in 6 passbands over a period of 10 years. Tomaximize the survey efficiency under variable atmosphericconditions (especially with changing cloud cover andvariable sky brightness) , we are implementing an all-skyoptical wavelength camera and associated image analysispipeline. This camera will take photos of the sky everyminute and return quantitative information about cloudcover to be used in informing the LSST scheduler. In thenearer term the all-sky data will inform the image andscheduler simulations that are being used to plan theproject. We present results from calibration andcharacterization of a Canon 5D Mark III camera in alaboratory setting, as well as preliminary results from sitesin Chile and Hawaii.Author(s): Michael Coughlin (Harvard University), Chuck Claver(National Optical Astronomy Observatory), Christopher Stubbs (HarvardUniversity), John Tonry (University of Hawaii)

122.18 – Polarimetric analysis of the ThirtyMeter Telescope (TMT) for modelinginstrumental polarization characteristicsBecause a polarimetric observing capability is an importantfunction that the Thirty Meter Telescope (TMT) will be calledupon to support, many different observing programscovering a range of different science areas are beingconsidered for the TMT and a model of the overallpolarization characteristics is being developed. Theinstrument development program will provide a means forpolarimetric instruments to be developed, however thetelescope itself and the AO system must be able to supportpolarimetric instruments. As a first step to defining thenecessary polarimetric technical requirements we havecreated an international working group to carry out a studyin which technical and cost implications will be balancedwith scientific impact; new requirements will be generatedwith supporting science cases. We present here initialresults of the instrumental polarization sensitivity of TMTwith NFIRAOS, the first-light adaptive optics system.Author(s): Warren Skidmore (Thirty Meter Telescope ObservatoryCorp.), Jenny Atwood (National Research Council Canada), RamyaManjunath (Indian Institute of Astrophysics), Krishna Reddy (ARIES), G.Anupama (Indian Institute of Astrophysics), Asoke Sen (Assam University)

Contributing teams: The TMT Polarimetry and TimeResolved Working Group

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122.19 – Early science performance andupcoming changes at Lowell Observatory'sDiscovery Channel TelescopeScience operations began in 2013 on Lowell Observatory'sDiscovery Channel Telescope (DCT). The DCT is a 4.3mtelescope designed and constructed for astronomicalobservations in the optical and near infrared. The f/6.1 RCfocus has an instrument cube with integrated wave frontsensing and guider systems, capable of carrying fiveinstruments. The first instrument, currently in use, is theLarge Monolithic Imager, a 6Kx6K optical CCD camera.Three spectrographs are under construction or modificationand are expected to commission on the telescope later in2014. The spectrographs are (1) the low to mid-resolutionoptical DeVeny spectrograph, being modified now in theLowell shop, (2) the Near IR High Throughput Spectograph(NIHTS), which is a low resolution spectrograph that willcover J through K bands in one observation and (3) theRapid IMager-Spectrometer (RIMAS) being built by theGoddard Space Flight Center and the University ofMaryland. The on-sky pointing and tracking performance ofthe telescope, have proven to be stable and repeatable.The active optics support system has also proven to be areliable performer. The first implementation of an open loopmodel of the optical aberrations, combined with thetracking are giving image quality in line with our hopesbased on the original site survey. Key milestones definingthe transition from commissioning to full operations areexpected to be complete by the end of 2014.Author(s): Stephen Levine (MIT)

Contributing teams: DCT Engineering Team, LowellInstrument Group

122.20 – Photometry and Spectroscopy withthe SMARTS Consortium TelescopesWe present recent results from the SMARTS ConsortiumTelescopes located at Cerro Tololo, designed to highlight thecapabilities of the telescopes and instruments. We willreport astrometry from the 0.9m+2KCCD obtained for theRECONS project (Dieterich et al. 2014 and Riedel et al.2014), optical/IR photometry obtained with the1.3m+ANDICAM for studies of X-ray binaries (e.g.MacDonald et al. 2014) and the SMARTS/Fermi blazarproject (Bonning et al. 2012), and high-resolutionspectroscopy obtained with the 1.5m+Chiron for exoplanetstudies (Tokovinin et al. 2013). We note that time isavailable to new private partners on all thesetelescope/instrument combinations.Author(s): Charles Bailyn (Yale Univ.), Michelle Buxton (Yale Univ.),Victoria Misenti (Yale Univ.), Debra Fischer (Yale Univ.), Todd Henry(Georgia State), Nicole Van Der Bliek (CTIO)

122.21 – Faster, Better, Cheaper: AZERODUR® low-expansion, light-weightpresent path toward affordable spacebornetelescopesFor competed missions, payload costs are often thediscriminate of whether or not outstanding science can beselected to fly. Optical Telescope Assemblies (OTAs)encompass a significant fraction of the payload cost, andmirror aperture and stability are usually are key to thescience merit. The selection of the primary mirror approachdrives architecture decisions for the rest of the OTA andeven payload. We look at the ways OTA architecture isaffected by the PM selection, and specifically at thebenefits of selecting a low expansion material. We will alsoreview recent advances in ZERODUR® fabrication whichmake this low-expansion material relevant in situationswhere affordable, lightweight mirrors can enable theapertures needed for science merit. Extreme LightweightZERODUR® Mirrors (ELZM) are available in apertures from0.3m to over 4m. SCHOTT has recently demonstrated arelevant 1.2m ELZM substrate.Author(s): Anthony Hull (University of New Mexico), ThomasWesterhoff (SCHOTT AG)

122.22 – Computational modeling ofRadioisotope Thermoelectric Generators(RTG) for interplanetary and deep spacetravelThis research project is part of Narsis Nejat Master ofScience thesis project that it is done at Shiraz University.The goals of this research are to make a computer model toevaluate the thermal power, electrical power, amount ofemitted/absorbed dose, and amount of emitted/absorbeddose rate for static Radioisotope Thermoelectric Generators(RTG)s that is include a comprehensive study of the typesof RTG systems and in particular RTG’s fuel resulting fromboth natural and artificial isotopes, calculation of thepermissible dose radioisotope selected from the above, andconceptual design modeling and comparison betweenseveral NASA made RTGs with the project computer modelpointing out the strong and weakness points for using thismodel in nuclear industries for simulation. The heat is beingconverted to electricity by two major methods in RTGs:static conversion and dynamic conversion. The model thatis created for this project is for RTGs that heat is beingconverted to electricity statically. The model approximatesgood results as being compared with SNAP-3, SNAP-19,MHW, and GPHS RTGs in terms of electrical power,efficiency, specific power, and types of the mission andamount of fuel mass that is required to accomplish themission.Author(s): Cyrus Nejat (University of Southern California), NarsisNejat (Shiraz University), Najmeh (Setareh) Nejat (Shiraz University)

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122.23 – The PockeQube T-LogoQube: aPrototype Approach for Future SpacedBased Astronomy ExperimentsT-LogoQube is a first generation 3P (size 5 cm x 5 cm x 15cm) ~500 gram PocketQube which flies instrumentation.The project is a collaboration between undergraduateuniversities Morehead State (MSU) in Kentucky and SonomaState (SSU) in California. The purpose of this project is todevelop a platform for future space-based scienceexperiments including astronomy. This first 3P satellite isone of the smallest, stand-alone satellites to send both aradio beacons and instrumentation telemetry. T-LogoQubesuccessfully reached orbit on November 21 in a sunsynchronous polar low-earth orbit. A Russian DNEPR-1

rocket from Dombarovsky Cosmodrome at Yasny, Russiacarried an Italian micro-satellite called Unisat-5 whichactually released the T-LogoQube satellite into space. Flightsoftware is written in the programming language microLogo(ulogo) which makes this satellite a platform for futurespaced-based astronomy experiments. The T-LogoQubeteam is comprised of about fifty people (professionalmentors, faculty, and students).Author(s): Aaron Owen (Sonoma State University), Kevin Zack(Sonoma State University), J. Jernigan (Little H-Bar Ranch), Bob Twiggs(Morehead State Univerisity), Lynn Cominsky (Sonoma State University),Benjamin Malphrus (Morehead State Univerisity), B. Silverman (PICO), S.McNeil (Little H-Bar Ranch), W. Roach-Barrette (Little H-Bar Ranch)

Contributing teams: and the T-LogoQube Team

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123 – SPD Posters 1Poster Session – Essex Ballroom and America Foyer – 02 Jun 2014 09:00 AM to 06:30 PM

123.01 – Absolute AbundanceMeasurements in Solar FlaresWe present measurements of elemental abundances insolar flares with EVE/SDO and EIS/Hinode. EVE observesboth high temperature Fe emission lines Fe XV-XXIV andcontinuum emission from thermal bremsstrahlung that isproportional to the abundance of H. By comparing therelative intensities of line and continuum emission it ispossible to determine the enrichment of the flare plasmarelative to the composition of the photosphere. This is thefirst ionization potential or FIP bias (F). Since thermalbremsstrahlung at EUV wavelengths is relatively insensitiveto the electron temperature it is important to account forthe distribution of electron temperatures in the emittingplasma. We accomplish this by using the observed spectrato infer the differential emission measure distribution andFIP bias simultaneously. In each of the 21 flares that weanalyze we find that the observed composition is close tophotospheric. The mean FIP bias in our sample isF=1.17+-0.22. Furthermore, we have compared the EVEmeasurements with corresponding flare observations ofintermediate temperature S, Ar, Ca, and Fe emission linestaken with EIS. Our initial calculations also indicate aphotospheric composition for these observations. Thisanalysis suggests that the bulk of the plasma evaporatedduring a flare comes from deep in the chromosphere, belowthe region where elemental fractionation in the non-flaringcorona occurs.Author(s): Harry Warren (Naval Research Lab.)

123.02 – Pre-Impulsive Flares andChromospheric Heating/EvaporationMechanisms with RHESSI and AIAWe present an investigation of RHESSI flares with a distinct"early rise" or "pre-impulsive" phase in which low-energyX-ray flux (6-12 keV) increases ~minutes before moreenergetic (25-50 keV), impulsive emission. It is currentlyunclear what the dominant heating mechanism is for thisclass of events; studies have claimed chromosphericheating by non-thermal electron beams or by conduction(see e.g. Siarkowski et al. 2009, Battaglia et al 2009). Weuse AIA data in conjunction with the data analysistechnique outlined in Brosius & Holman 2012 to distinguishbetween chromospheric heating/evaporation mechanisms.This technique involves the temporal analysis of AIAlightcurves in the passbands sensitive to flaretemperatures; a simultaneous increase in all channels isinterpreted as beam-driven chromospheric heating,whereas an early increase in hotter channels can indicate ahot coronal source and conductive heating. RHESSI imagingand spectroscopy is performed to determine flareparameters such as temperature, density, and power-lawindex (if a detectable non-thermal component is present).We also perform a search for early phase, non-thermalcoronal sources similar to those observed in some strongevents such as 2002 July 23.Author(s): Andrew Marsh (UC Santa Cruz), David Smith (SpaceSciences Laboratory, UC Berkeley), Lindsay Glesener (Space SciencesLaboratory, UC Berkeley), Amir Caspi (Laboratory for Atmospheric andSpace Physics, Univ. of CO)

123.04 – Study of Two Successive Three-ribbon Solar Flares Using BBSO/NSTObservationsWe studied two rarely observed three-ribbon flares (M1.9and C9.2) on 2012 July 6 in NOAA AR 11515, which wefound using H? observations of 0.1 arcsec resolution fromthe New Solar Telescope and Ca II H images from Hinode.The flaring site is characterized by an intriguing "fish-bone-like" morphology evidenced by both Halpha imagesand a nonlinear force-free field (NLFFF) extrapolation,where two semi-parallel rows of low-lying, sheared loopsconnect an elongated, parasitic negative field with thesandwiching positive fields. The NLFFF model also showsthat the two rows of loops are asymmetric in height andhave opposite twists, and are enveloped by large-scale fieldlines including open fields. The two flares occurred insuccession within half an hour and are located at the twoends of the flaring region. The three ribbons of each flarerun parallel to the magnetic polarity inversion line, with theouter two lying in the positive field and the central one inthe negative field. Both flares show surge-like flows inHalpha apparently toward the remote region, while theC9.2 flare is also accompanied by EUV jets possibly alongthe open field lines. Interestingly, the 12-25 keV hard X-raysources of the C9.2 flare first line up with the central ribbonthen shift to concentrate on the top of the higher branch ofloops. These results are discussed in favor of reconnectionalong the coronal null line, producing the three flare ribbonsand the associated ejections.Author(s): Haimin Wang (NJIT), Chang Liu (NJIT), Na Deng (NJIT),Zhicheng Zeng (NJIT), Yan Xu (NJIT), Ju Jing (NJIT), Wenda Cao (NJIT)

123.05 – Magnetic Field Changes inSDO/HMI Line-of-sight Magnetogramsduring Large Solar FlaresPhotospheric magnetic fields are often used to study thetopology of a flaring active region as well as to predictwhen a flare will happen. We examined SDO/HMIline-of-sight magnetograms for forty flares (M5.0 or larger)from 2010 to 2013. Using the full-resolution (0.5arcsecond/pixel) and high time cadence (45-second),observations, we identified three types of changes inline-of-sight magnetic flux near the flaring region duringlarge solar flares: First, discreet jumps or steps in theline-of-sight magnetic flux are often observed whenexamining magnetograms before and after the flare.Second, spikes or rapid and transient changes lasting just afew minutes occur during the rise of the flare, coincidingwith the impulsive phase. Finally, in a few flares,moderate-scale waves in magnetograms, similar toMoreton or EIT waves, are seen propagating away from theflaring region. In this study, we provide statistics on thesedifferent apparent magnetic flux changes as well as offerpossible physical explanations.Author(s): K. Balasubramaniam (USAF/AFRL), Rachel Hock(USAF/AFRL)

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123.06 – Magnetic Energy Dissipation in 200Solar Flares Measured with SDOWe present the first statistical study of magnetic energeticsin solar flares. The amount of dissipated magnetic energyduring solar flares provides the fundamental limit on theflare energy budget that is partitioned into the kinetic andpotential energy of CMEs, acceleration of nonthermalparticles, and radiation in soft X-rays, EUV, UV, andbolometric luminosity. The determination of the dissipatedmagnetic energy requires the calculation of nonlinearforce-free field (NLFFF) solutions during flares, which canquantify the nonpotential E_N(t), the potential E_P(t), andthe free magnetic energy E_{free}(t)=E_N(t)-E_P(t), whichitself represents an upper limit on the magnetic energydE_diss that can be dissipated during a flare. Here wedeveloped a NLFFF forward-fitting code that fits anonpotential field in terms of vertical currents with helicallytwisted field lines to automatically traced coronal loopsfrom 7 AIA wavelength filters and apply it to 200 M- andX-class flares that have been observed during the first 4years of the Solar Dynamics Observatory (SDO) mission.We cacluate the free energy with a cadence of 6 minutesduring all 200 flares, and find significant magnetic energydecreases dE_diss in almost all flares, in the order of E_diss~ 10(31)-10(32) erg, which amounts to a fraction ofdE_diss/E_P ~ 0.01-0.3 of the potential magnetic energyE_P. We find that the dissipated energy dE_diss cannotsimply be determined by an energy difference before andafter the flare, because the hydrodynamic evolution causesbrightenings and dimmings of helically twisted loops(sigmoids) in the flare core region, which acts as atime-dependent illumination effect of nonpotential loopstructures.Author(s): Markus Aschwanden (Lockheed Martin ATC)

Contributing teams: AIA/SDO

123.07 – The Multi-Instrument,Comprehensive Differential EmissionMeasure (DEM) of the Solar Corona DuringFlares and Quiescent PeriodsThermal plasma in the solar corona, while often modeled asisothermal for ease of analysis, is in fact decidedly multi-thermal, ranging from ~1-2 MK in the quiescent corona to~30-50 MK in intensely flaring loops. It has proven difficultto obtain a well-constrained differential emission measure(DEM) from a single instrument, as the wavelength rangesof individual instruments, even those with broadbandcoverage, provide sensitivity to only a limited range ofplasma temperatures. Recently, we developed a newtechnique using combined extreme ultraviolet (EUV) andsoft and hard X-ray (SXR, HXR) data from the EUVVariability Experiment (EVE) onboard the Solar DynamicsObservatory (SDO) and the Reuven Ramaty High EnergySolar Spectroscopic Imager (RHESSI), respectively, toobtain a self-consistent DEM that is strongly constrainedacross the full range of coronal plasma temperatures (<2 to>50 MK). An accurate, precise determination of the plasmatemperature distribution enables not only studies of plasmaheating and thermal plasma evolution, but can also providestrong constraints on the non-thermal accelerated electronpopulation, including the low-energy cutoff which istypically determined only as a loose upper limit. We presentEVE+RHESSI DEM results from selected intense (X-class)flares from solar cycle 24, including determining thenon-thermal low-energy cutoff and examining how thisevolves with the temperature distribution. We also applythis technique to combine EUV data from EVE with SXRdata from the GOES X-ray Sensor (XRS) and the X123, anew SXR spectrometer flown on two recent SDO/EVEcalibration sounding rockets, to examine the DEM duringquiescent (non-flaring) times with varying activity levels;the X-ray data provide crucial constraints on thehigh-temperate extent of the DEM and any potentialnon-thermal emission. We compare these results with thosefrom a parallel technique to derive DEMs from imaging datafrom the Atmospheric Imaging Assembly (AIA) onboardSDO, and we discuss the implications for plasma heating,both during flares and in the quiescent corona. Thisresearch is supported by NASA contracts NAS5-98033 andNAS5-02140, and NASA Heliophysics Guest InvestigatorGrant NNX12AH48G.Author(s): Amir Caspi (University of Colorado), James McTiernan(University of California), Harry Warren (Naval Research Laboratory),Thomas Woods (University of Colorado)

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123.08 – Searching for narrow-bandoscillations in solar flares in the presence offrequency-dependent noiseA common feature of solar flare emission is the appearanceof short timescale fluctuations, often interpreted in terms ofoscillatory signatures, and often referred to as quasi-periodic pulsations (QPPs) or quasi-periodic oscilations(QPOs). These fluctuations are an important diagnostic ofsolar plasma, as they are linked to the flare reconnectionand particle acceleration sites. However, it has recentlybecome clear that solar flare time series, like manyastrophysical objects, are often dominated by frequency-dependent 'red' noise, rather than white noise. Thisfrequency-dependent red-noise is commonly not taken intoaccount when analyzing flare time-series for narrow-bandoscillations. We demonstrate the application of a Bayesianmethod of searching for narrow-band oscillations in flares(based on Vaughan 2010) that fully accounts for frequency-dependent noise. We apply this method to the recent flaresof 2011 February 15 and 2011 June 7, utilizinghigh-cadence EUV and X-ray data from the Proba-2/LYRAand Fermi/GBM instruments. While emphasizing that theobserved fluctuations are a very real effect, we show thatthe emission from the selected events can be welldescribed by a frequency-dependent noise model, withoutthe need to invoke an explicit oscillatory mechanism. Thispresents a challenge to our current understanding of flarefluctuations, and suggests that narrow-band oscillations inflare emission may be much less prevalent than previouslybelieved.Author(s): Andrew Inglis (NASA Goddard Space Flight Center), JackIreland (NASA Goddard Space Flight Center)

123.09 – A FLARE OBSERVED IN CORONAL,TRANSITION REGION AND HELIUM I 10830 ÅEMISSIONSOn June 17, 2012, we observed the evolution of a C-classflare associated with the eruption of a filament near a largesunspot in the active region NOAA 11504. We obtained highspatial resolution filtergrams using the 1.6 m New SolarTelescope at the Big Bear Solar Observatory in TiObroad-band (bandpass: 10 Å)and He I 10830 Å narrow-band(bandpass: 0.5 Å, centered 0.25 Å to the blue). We analyzethe spatio-temporal behavior of the He I 10830 Å data,which were obtained over a 90×90 arcsends field of viewwith a cadence of 10 sec. We also analyze simultaneousdata from the Atmospheric Imaging Assembly and ExtremeUltraviolet Variability Experiment instruments on board theSolar Dynamics Observatory spacecraft, and data fromReuven Ramaty High Energy Solar Spectroscopic Imagerand GOES spacecrafts. Several quantitative aspects of thedata, as well as models derived using the “0D”Enthalpy-Based Thermal Evolution of Loops model (EBTEL:Klimchuk et al. 2008) code, indicate that the 10830 Åmultiplet is formed primarily by photoionization ofchromospheric plasma followed by radiative recombination.Surprisingly, the He II 304 Å line is reasonably well matchedby standard emission measure calculations, along with theC IV emission which dominates the AIA 1600 Å channelduring flares. This work lends support to some of ourprevious work combining X-ray, EUV and UV data of flaresto build models of energy transport from corona tochromosphere.Author(s): Zhicheng Zeng (Big Bear Solar Observatory), Jiong Qiu(Montana State University), Wenda Cao (Big Bear Solar Observatory),Philip Judge (High Altitude Observatory)

123.10 – Sub-arcsecond Structure andDynamics of Flare Ribbons Observed withNew Solar TelescopeEmission of solar flares across the electromagneticspectrum is often observed in the form of two expandingribbons. The standard flare model explains the flare ribbonsas footpoints of magnetic arcades, emitting due to theinteraction of energetic particles with the chromosphericplasma. However, the physics of this interaction andproperties of the accelerated particles are still unknown.We present results of multiwavelength observations of C2.1flare of August 15, 2011, observed with the 1.6-meter NewSolar Telescope of Big Bear Solar Observatory. Theseunique data are characterized by the great spatialresolution reaching the telescope diffraction limit with goodspectral scanning of H-alpha line, and photosphericimaging. The observations reveal previously unresolvedsub-arcsecond structure of the flare ribbons in regions ofstrong magnetic field. We discuss the fine structure of theflare ribbons, their dynamics, and possible mechanisms ofthe energy release and transport, using also data fromSDO, GOES and FERMI spacecraft.Author(s): Ivan Sharykin (Space Research Institute of RAS),Alexander Kosovichev (Stanford University)

123.11 – Helioseismic and Magnetic ImagerObservations of Linear Polarization from aLoop Prominence SystemWhite-light observations by the Solar DynamicsObservatory's Helioseismic and Magnetic Imager of aloop-prominence system occurring in the aftermath of anX-class flare on 2013 May 13 near the eastern solar limbshow a linearly polarized component, reaching up to 20% atan altitude of 33 Mm, about the maximal amount expectedif the emission were due solely to Thomson scattering ofphotospheric light by the coronal material. The massassociated with the polarized component was 8.2x10^14 g.At 15 Mm altitude, the brightest part of the loop was3(+/-0.5)% linearly polarized, only about 20% of thatexpected from pure Thomson scattering, indicating thepresence of an additional unpolarized component atwavelengths near Fe I (617.33 nm), probably thermalemission. We estimated the free electron density of thewhite-light loop system to possibly be as high as1.8x10^12 cm^-3.Author(s): Pascal Saint-Hilaire (University of California, Berkeley),Jesper Schou (Max-Planck-Institut fur Sonnensystemforschung), JuanCarlos Martinez Oliveros (University of California, Berkeley), Hugh Hudson(University of Glasgow), Sam Krucker (University of Applied Sciences andArts Northwestern Switzerland), Hazel Bain (University of California,Berkeley), Sebastien Couvidat (Stanford University)

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123.12 – Acceleration Regions JointlyObserved with Microwave and X-RayImaging Spectroscopy in a Number of SolarFlaresDetection of acceleration regions in solar flares has provedchallenging for many reasons, in particular, because theX-ray emission is weighted by denser regions of the flarevolume, although the acceleration can take place in atenuous region, while the microwave emission, which canbe significant even from the tenuous regions, is oftendominated by a (looptop) trapped population, rather thanthe acceleration region itself. For these reasons weundertook a systematic database search to identify eventsthat do not show a significant trapped component and atthe same time show evidence of the source uniformity,which simplifies the data analysis greatly. Initially, weidentified a subset of more than 20 radio bursts with arelatively narrow spectrum, having the low- and high-frequency spectral indices larger than 3 by the absolutevalue. That steep low-frequency spectrum implies that theemission is nonthermal (for the thermal emission thespectral index is supposed to be 2 or flatter), and thesource is reasonably dense and uniform. The steephigh-frequency spectrum implies that no significantelectron trapping occurs; otherwise a progressive spectralflattening would be observed. Roughly half of these radiobursts have RHESSI data, which allows for a detail jointdiagnostics of the source parameters and evolution. Basedon the studied radio-to-X-ray spatial relationships, timing,and spectral fits we do conclude that we deal here withemission from directly the acceleration regions. We discussthe implications of these observations for the accelerationmechanism involved. We also discuss further strategy ofhow to detect the acceleration region with the currentlyavailable observational means. This work was supported inpart by NSF grants AGS-1250374, and NASA grantsNNX11AB49G and NNX14AC87G to New Jersey Institute ofTechnology.Author(s): Gregory Fleishman (NJIT), Eduard Kontar (University ofGlasgow), Gelu Nita (NJIT), Dale Gary (NJIT)

123.13 – Heating Rate in ReconnectionFormed Flare LoopsHigh-resolution ultraviolet (UV) and extreme ultraviolet(EUV) images of solar flares have revealed that flare loopsare formed by magnetic reconnection events successivelyand heated separately. Our recent work (Qiu et al. 2012)suggests that the heating rate in individual flare loopscould be inferred from the rapid rise of UV brightness at thefoot-points of these loops. The heating rate is furtherrestricted by comparing the observed coronal radiation andthe synthetic one from plasma in all these loops computedby the Enthalpy-Based Thermal Evolution of Loops (EBTEL,Klimchuk et al. 2008, Cargrill et al. 2012) model. Therefore,the method uses observations to constrain the heatingrates from both the input and output of the loop heatingmodel. In this study, we apply this method to three flares ofdifferent magnitude, respectively. Comparison of the resultsfrom the three events show that the synthetic coronalradiation compares reasonable well with observations fromplasma with temperature in the range of 3-10MK. Thisexperiment provides another independent constraint todetermination of the heating rates. Furthermore, usingRHESSI hard X-ray observations, we also infer the fractionof non-thermal beam heating in the total heating rate offlare loops, and discuss its effect on plasma evolution. Forthe 2005 May 13 M8.0 flare that exhibits significant thick-target hard X-ray emissions, the lower limit of the totalenergy used to heat the flare loops is 1.2e31 ergs, out ofwhich, less than 20% is carried by beam-driven upflowsduring the impulsive phase.Author(s): Wenjuan Liu (Montana State University), Jiong Qiu(Montana State University), Dana Longcope (Montana State University),Amir Caspi (University of Colorado)

123.14 – Relationship between unusualfeatures in umbrae and flaresThe influence of photospheric and chromospheric dynamicsand morphologies on flare activity are still unclear. Wepresent a study of two flaring active regions (ARs) withcomplementary instruments (DST/IBIS, Hinode/SOT-SP,SDO/HMI and SDO/AIA) to investigate the temporalevolution of the sunspots and their magnetic andthermodynamic properties. In spite of vast differences inflare occurrence and flare magnitudes, both ARs showsimilar features in the lower solar atmosphere during flares.We investigate common magnetic topologies anddynamics, which may favor flare activity.Author(s): Alberto Sainz Dalda (Stanford-Lockheed Institute forSpace Research), Lucia Kleint (BAER Institute)

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123.15 – Decay-phase Cooling and InferredHeating of M- and X-class Solar FlaresHydrodynamic modelling is a well established andimportant field in understanding the evolution of solarflares. However, in order to be of greatest use the results ofsuch models must be compared to statistically significantsamples of flare observations. In this talk weobservationally investigate the hydrodynamic decay phaseevolution of 72 M- and X-class flares using GOES/XRS,SDO/EVE and Hinode/XRT and quantify their cooling rates.The results are then compared to the predictions of ananalytical zero-dimensional hydrodynamic model. We findthat the model does not fit the observations well, but doesprovide a well-defined lower limit on a flare's total coolingtime. The discrepancy between observations and the modelis then assumed to be primarily due to heating during thedecay phase. The decay-phase heating necessary toaccount for the discrepancy is quantified and found be~50% of the total thermally radiated energy, as calculatedwith GOES/XRS. This suggests that the energy releasedduring the decay phase may be as significant as thatreleased during the rise phase.Author(s): Daniel Ryan (Trinity College Dublin), Phillip Chamberlin(NASA Goddard Space Flight Center), Ryan Milligan (Catholic University ofAmerica), Peter Gallagher (Trinity College Dublin)

123.16 – A study of sympathetic eruptionsusing the Heliophysics EventsKnowledgebaseOver the past few decades there have been a number ofpapers investigating the connection between flaresoccurring in succession. Statistically, any connection thataffects the timing of successive flares that exists is found tobe weak. However, the majority of previous investigationshas been limited by only considering the causal connectionbetween soft X-ray flares. More recent case studies haveshown convincing evidence that large eruptions cause aglobal reorganization of overlying magnetic fields that canresult in the eruption of both flares and filaments at largedistances from the original event. In this work, theconnection between GOES X-ray flares (C-, M-, and X-class)and filament eruptions occurring in succession in twodifferent active regions is considered statistically. Thefilament eruptions are recorded in the Heliophysics EventsKnowledgebase by observers using SDO/AIA data. Asignificant causal connection is found between the twoevent types, such that large flares are followed by filamenteruptions within 24 hours much more often than they arepreceded by filament eruptions. This stipulates that theflares either cause the filaments to erupt or affect theeruption timing such that the filament eruptions follow theflares more closely in time.Author(s): Paul Higgins (Lockheed Martin), Carolus Schrijver(Lockheed Martin), Alan Title (Lockheed Martin), D. Shaun Bloomfield(Trinity College Dublin), Peter Gallagher (Trinity College Dublin)

123.17 – Different Temperature Evolution InMagnetic Flux Rope and Near-Surface FlareLoop Source In A Failed Solar EruptionSolar eruption is a transient energetic phenomenon thatinvolves sophisticated kinematic, morphological andthermal evolution. The observed evolution bears theknowledge on the physical mechanism of solar eruptions.Here we report a detailed study of a failed solar eruptionoccurred on January 05, 2013, which generated an M1.7X-ray flare and a giant "fire ball" that likely represent amagnetic flux rope. The flux rope, a well-organizedstructure in the corona, was initially impulsively acceleratedto a speed of $\sim$400 km/s in the first minute, thendecelerated and came to a complete stop in two minutes.The failed eruption resulted in a large-size high-lying($\sim$100 Mm above the surface) high-temperature ``fireball" sitting in the corona for more than two hours. The timeevolution of the thermal structure of the flux rope wasrevealed through the differential emission measure analysistechnique, which produced temperature maps usingobservations of the Atmospheric Imaging Assembly onboard \textit{Solar Dynamic Observatory}. The averagetemperature of the flux rope steadily increased from$\sim$5 MK to $\sim$10 MK during the first nine minutes ofthe evolution. On the other hand, the temperature increaseof the near surface flare loop source lasted only threeminutes, similar to the rise time of the associated soft X-rayflare. We suggest that the flux rope is heated by thethermal energy release of the continuing magneticreconnection in the high corona, which is different from theheating of the low-lying flare loops. The low-lying loops arelikely heated by chromospheric plasma evaporation duringthe flare main phase. The large ambient loops overlying theflux rope was pushed up by $\sim$10 Mm during theattempted eruption. The pattern of the velocity variation ofthe ambient loops strongly suggests that the failure of theeruption is caused by the strapping effect of the overlyingloops.Author(s): Jie Zhang (George Mason Univ.), Hong-qiang Song (GeorgeMason Univ.)

123.18 – The Study of Solar EnergeticProtons Associated with EUV WavesWe studied the relationship between solar energeticprotons (SEPs) and extreme ultraviolet (EUV) waveproperties between 2010 August and 2013 May observedby STEREO, SOHO and SDO. We determined the onsettimes, peak times and peak fluxes of the SEPs in SOHOERNE and STEREO LET proton channel (6 – 10 MeV). FullSun heliographic images created by combining STB 195Å,SDO 193Å, and STA 195Å were used for the analysis of theEUV waves. EUV wave arrival times at the spacecraftconnecting points and their speed on the low corona weredetermined by space-time plots. It is noted that there is asignificant correlation between the EUV wave arrival timesand SEP onset times (r=0.73) but no SEP peak times. SEPpeak fluxes increase with EUV wave speed (r=0.69) and thepower law spectral index become harder with the EUV wavespeed. This suggests that energetic protons are stronglyassociated with EUV waves, which is considered as thesignature of CME shock in the low corona.Author(s): Jinhye Park (Kyung Hee University), Davina Innes (MaxPlanck Institute), Radoslav Bucik (Max Planck Institute), Yong-Jae Moon(Kyung Hee University), Stephen Kahler (Air Force Research Laboratory)

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123.20 – IRIS Observations of the SolarAtmospheric Response to FlaresThe Interface Region Imaging Spectrograph (IRIS) is a NASASmall EXplorer mission to observe the sun. It observes highresolution images and spectra in the chromospheric C IIand Mg II lines, the transition region Si IV and O IV lines,and the coronal XXI line. Since its launch on June 27 2013,IRIS has observed several solar flares. The high spatialresolution of IRIS, and its range of spectral lines allow adetailed analysis of the flare energy deposition and flaredynamics in the lower solar atmosphere, especially inconjunction with complementary observations from SDO,Hinode, and RHESSI. We present initial IRIS observations ofthe solar flare response in a broader observational contextand discuss how IRIS can provide new insight into the flareprocess.Author(s): Jean-Pierre Wuelser (Lockheed Martin ATC)

Contributing teams: The IRIS team

123.21 – Chromospheric Magnetic Fields inthe X1.2 Flare of January 7, 2014Measurements of magnetic fields in chromospheric flaresare scarce and many basic magnetic properties of flares areuncertain. A four-ribbon X1.2 flare occurred near diskcenter on January 7, 2014. It was observed at the time ofpeak soft X-ray emission with the NSO SOLIS vectorspectromagnetograph using the 854.2 nm line of Ca II. Afull vector modulator for this wavelength is underconstruction, but for this observation only intensity (I) andcircularly polarized (V) spectral line profiles were obtained.Given the large variations of physical properties along sightlines through the chromosphere, especially in a flare, it isdifficult to measure the magnetic field. We apply threesimple techniques to estimate chromospheric andphotospheric average flux densities. One method uses thewavelength difference between selected portions of the I±Vline profiles. A second method integrates |V/I| over portionsof the line profile. A third method uses the simpleweak-field approximation, V ? dI/d?, but with modificationsto the observed I profile to better match the V profile. As iswell known in flares, there are asymmetry and line widthvariations in the emission and absorption line profilesindicating complicated mass motions along lines of sight. Atentative conclusion is that in most areas of the flare theaverage magnetic flux density along the line of sight is verysimilar to the underlying photosphere but usually weaker.Obtaining more robust measurements and conclusionsrequires exploration by forward modeling of theobservations with realistic model atmospheres. Usefulinversions may someday be possible if the atmospheremodel parameters to be fit can be restricted enough tomatch the information content of the observed spectra.Author(s): J. Harvey (National Solar Obs.)

Contributing teams: SOLIS Team

123.22 – The Formation of AcceleratedElectron Distributions in Solar FlaresDriven by RHESSI observations of dense compact coronalhard X-ray sources in solar flares, we study electronacceleration in such regions. We consider the accelerationof electrons by a stochastic process that is characterized bya diffusion coefficient D_turb ~ 1/v in a collisional mediumof finite length. If electron escape can be neglected, theelectron distribution function is determined by a balancebetween stochastic acceleration and collisional friction.Such a scenario admits a stationary solution for theelectron distribution function that takes the form of akappa-distribution. We show how the growth toward thisstationary distribution can be described as a "wave"'propagating forwards in velocity space, so that electrons ofhigher energy E are accelerated later than lower-energyones; quantitatively, the acceleration time ? scales with Eaccording to ? ~ E^{3/2}. Since such an approach towardsa stationary kappa distribution becomes progressivelyslower at high energies, escape from the accelerationregion (of finite length L) will, at sufficiently high energies,eventually dominate over collisions, and a differentstationary solution, corresponding to a balance betweendiffusive acceleration and particle escape, is applicable inthis energy range. Using a numerical treatment, we derivethe time evolution toward the stationary solution for arange of parameters appropriate to the solar flare situation.Author(s): A. Emslie (Western Kentucky University), Nicolas Bian(University of Glasgow), Eduard Kontar (University of Glasgow)

123.23 – Element Abundances inHigh-temperature Solar Flare Plasma fromMESSENGER SAX ObservationsX-ray spectral measurements of many solar flares madewith the MESSENGER SAX instrument have been used todetermine the abundances of Fe, Ca, Ar, S, and Si in thehigh temperature plasma. All available data from launch in2004 to date have been used to obtain spectral fits to theSAX data from 2.3 to 8.5 keV for all time intervals with adetectable count rate in the Fe-line complex at 6.7 keV. Foreach time interval, OSPEX, our object-oriented IDL spectralanalysis program, is used to obtain values of the emissionmeasure, temperature distribution, and abundances thatgive the best-fit of the corresponding CHIANTI photonspectrum folded through the instrument response matrix tothe measured count-rate spectrum above background.Distributions will be presented of element abundances foreach flare and for all flares detected during each year ofobservations. Variations in measured abundances will bediscussed as to whether they reflect real differences fromthe mean or differences due to statistical and/or systematicuncertainties. Comparisons will be made with abundancemeasurements made from other data sets, in particular byPhillips and Dennis (2012) using data from the Ramaty HighEnergy Solar Spectroscopic Imager (RHESSI), and byWarren et al. (2013) using data from the EUV VariabilityExperiment (EVE) on the Solar Dynamics Observatory(SDO). Phillips, K. J. H. and Dennis, B. R., “The Solar FlareIron Abundance,” 2012, ApJ, 748, 52. Warren, H.“Measurements of Absolute Abundances in Solar Flares,”2013, arXiv, 2013arXiv1310.4765WAuthor(s): Brian Dennis (NASA's GSFC), Larry Nittler (CarnegieInstitution of Washington ), Kenneth Phillips (Natural History Museum),Richard Schwartz (The Catholic University of America), Richard Starr(NASA's GSFC), Anne Tolbert (The Catholic University of America)

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123.24 – Modeling the response of thelower atmosphere to flare reconnectionIt has long been recognized that energy release in a solarflare gives rise to ablation of material from thechromosphere (more commonly called evaporation). Theprevailing view is that energy is initially transformed fromstored magnetic energy by the process of magneticreconnection. In some models reconnection accelerateselectrons, either directly or indirectly, and thesenon-thermal electrons carry energy to the chromosphericfootpoints. In others the reconnection converts magneticenergy into heat in the corona and thermal conductioncarries that heat to the chromosphere. While nocomprehensive, self-consistent model yet exists for theconversion of magnetic energy to non-thermal electronenergy, models of the conversion to heat, via slowmagnetosonic shocks, have been available since Petschek's1964 paper. We present a numerical model encompassingthe conversion of magnetic energy to shocks, to heat, andthen to conduction-driven evaporation. We compare itsresults to those of more traditional conduction-drivenmodels where reconnection is replaced by an ad hocplasma heating. We consider, in particular, observablesignatures such as doppler shifts and formation of flareribbons. This work was supported by the NASA SR&Tprogram.Author(s): Dana Longcope (Montana State Univ.), Jiong Qiu (MontanaState Univ.), James Klimchuk (NASA GSFC, Code 671)

123.25 – Long Duration Flare Emission bySequential Reconnection and HeatingLong duration flare emissions lasting for a few hours arelikely produced by magnetic reconnection that continuouslyforms flare loops and heats plasma inside. In this study, wedemonstrate that this process leads to the long durationemission in a C2.9 flare on 2011 September 13. Observedby AIA, the flare exhibits an organized pattern of evolutionwith UV brightenings in flare ribbons spreading along thepolarity inversion line, followed by sequential formation ofpost-flare loops seen in EUV emissions. The spatiallyresolved observation of flare ribbons can be used to inferheating rates in sequentially formed and heated flare loops,with which we synthesize flare emission in these loops withhydrodynamic models. The 0d EBTEL model (Klimchuk et al.2008) efficiently computes mean properties of thousands offlare loops identified from flare ribbon signatures, and thesynthetic tempo-spatial evolution of the total emission is inreasonable agreement with EUV observations. The 1dmodel applied on a few selected loops reveals physics ofthe heating mechanism and along-the-loop dynamics,particularly during the impulsive heating phase. During thefour hours of this event, the estimated total energy in theheating amounts to 2e30 erg, with the total reconnectionflux about 1e21 Mx.Author(s): Jiong Qiu (Montana State University), Dana Longcope(Montana State University), James Klimchuk (NASA Goddard Space FlightCenter)

123.26 – Formation and Properties ofMagnetic Island Plasmoids in Large-ScaleCurrent Sheets During CME EruptionsWe present the continued analysis of the high-resolution2.5D MHD simulations of sympathetic magnetic breakouteruptions from a pseudostreamer source region. Weexamine the generation of X- and O-type null points duringthe current sheet tearing and their evolution asreconnection progresses. There are three large-scalecurrent sheets that we investigate in detail over the courseof the simulation. We examine the properties ofreconnection occurring within these current sheetsincluding evolution of the current sheet lengths, Lundquistnumber, and reconnection rates. We also quantify thestatistical and spectral properties of the fluctuations in thecurrent sheets resulting from the resistive tearing andmagnetic island plasmoid formation including thedistribution of magnetic island width, flux content, andmass. We show that the temporal evolution of the spectralindex of the magnetic energy density in our current sheetsappears to reflect the transition from the linear tonon-linear phase of the instability. Our results are inexcellent agreement with recent dedicated reconnectionsimulations even though our current sheets’ formation,growth, and dynamics are both dictated by and in turn,govern the global evolution of sequential, sympathetic CMEeruptions.Author(s): Benjamin Lynch (Univ. of California-Berkeley), JustinEdmondson (Univ. of Michigan)

123.27 – White-Light Observations of MajorFlares Compared to Total Solar Irradianceand Short-Wavelength ObservationsThe NSO’s GONG network produces “white light” (WL)continuum intensity images from one-minute integrationsaveraged across a 0.7~\AA\ wide band pass centered at6768~\AA\ at one minute cadence using six sitesworldwide. Clear WL signatures of solar flares are present inGONG intensity data for only the largest flares because oflow spatial resolution (2.5 arcsec pixel size). For six majorflares (GOES class X6.5 - X28) observed by GONG, wecompare integrated GONG full-disk WL intensity curves withSORCE/TIM total solar irradiance (TSI) measurements.Distinctive p-mode signatures are evident in both GONGand SORCE time series, though the correlation betweenGONG and SORCE data varies from flare to flare. In somecases a clear TSI peak and an interruption of the GONGp-mode pattern accompany the flare. The flare signature isgenerally weaker in the GONG data, suggesting that mostof the TIM flare signal arises from wavelengths shorter thanthe GONG band pass. The flare kernels nevertheless areclear and last many minutes in the spatially resolved GONGimage time series. We also compare the GONG activeregion intensity observations with shorter-wavelength data.In one case observed by TRACE, the GONG and TRACE WLcurves are very similar and the TRACE 1600~\AA\ curveshows a significant precursor and a long tail. In most casesthe GONG WL and RHESSI 25-100 keV counts appear wellcorrelated in time. This work utilizes GONG data obtainedby the NSO Integrated Synoptic Program (NISP), managedby the National Solar Observatory, which is operated byAURA, Inc. under a cooperative agreement with theNational Science Foundation.Author(s): Gordon Petrie (NSO), Greg Kopp (University of Colorado), J.Harvey (NSO)

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123.28 – Relating photospheric magneticfield changes and hard X-ray emissionduring flaresWe study the correlation between abrupt permanentchanges of magnetic field during strong flares observed byGONG and HMI instruments, and the location of hard X-ray(HXR) emission observed by RHESSI to relate the fieldchanges to the reconnection processes in the corona andinvestigate the origin of the field changes. Thechromospheric HXR emission in solar flares is generallyregarded as the footprints of magnetic field lines newlyreconnected in the corona. Also, the footpoint motionstraveling away from the neutral lines are considered to beindicative of the reconnection occurring in arcade magneticfields of increasing heights. Our analysis of six flares showsthat the early HXR emission corresponds well to locations ofthe strong field changes. The later HXR emission does notcorrespond to significant field changes as the footpoint ismoving away from the neutral line in later stages of theflare. The field changes and HXR emission are spatio-temporally related, but not simultaneous. The field changesstart earlier and end later than the detectable HXR signal.The strongest X-class flares in our analysis show awell-defined peak in the field changes a few minutes earlierthan the peak in the HXR emission. The timing relationshipbetween the HXR and the largest photospheric fieldchanges may indicate an indirect physical relationshipbetween these phenomena. Tracing of the field changes atthe footpoints’ locations shows that in most of the flaresthe field changes propagated at a speed similar to that ofthe HXR footpoint moving away from the neutral line.However most of the field changes occurred earlier in time.O.B., G.P. and A.P. are partially supported by NASA grantNNX14AE05G.Author(s): Gordon Petrie (NSO), Olga Burtseva (NSO), Juan CarlosMartinez Oliveros (UC Berkeley), Alexei Pevtsov (NSO)

123.29 – Investigating a Complex X-classSolar Flare Using Magnetic Field ModelingWe will present the investigation of a complex X-class flareoccurred in NOAA Active Region 11283 on 2011 September6. This flare is associated with two filament eruptions and acoronal mass ejection (CME) with speed of 575 km/s.AR11283 contains mainly two bipoles, a large decayingbipole and a small “L” shape emerging bipole with sunspots.The main eruption initiated and occurred in the smallbipolar region. Multiple flare ribbons are observed duringthe eruption. We studied the structure and dynamics of theerupting filaments and flare ribbons observed by SDO/AIAand Hinode/XRT as well as the dynamics of thephotospheric magnetic fields observed by SDO/HMI. Wealso constructed magnetic field models using the flux ropeinsertion method, in order to understand how the eruptionis triggered and how the flare ribbons are formed duringthe eruption.Author(s): Yingna Su (Harvard-Smithsonian Center forAstrophysics), Blake Forland (Harvard-Smithsonian Center forAstrophysics), Adriaan Van Ballegooijen (Harvard-Smithsonian Center forAstrophysics), Li Feng (Purple Mountain Observatory, CAS), Haisheng Ji(Purple Mountain Observatory, CAS)

123.30 – Distinguishing Between Supra-Arcade Downflows and PlasmoidsSupra-arcade downflows (SADs) observed above flaringactive regions during long-duration events are theorized tobe signatures of magnetic reconnection. Observations ofSADs strongly indicate an association with shrinkingreconnected flux tubes characterized by a specificmagnetic topology. Plasmoids comprise another proposedgroup of obserational reconnection signatures. While someplasmoids occur under nearly the same conditions as SADs,the magnetic configuration of the two phenomena are quiteincongruous, yet they are often categorized together. Wepresent distinguishing characteristics between SADs andplasmoids and indicate how their respective observationsmay yield insight into the conditions within the currentsheet above eruptive active regions.Author(s): Sabrina Savage (NASA/MSFC)

123.31 – Chromospheric and Coronal HMIFlare SourcesWe present observations of white-light features in the lowcorona, for three flares SOL20110308T1935,SOL20110308T0230 and SOL2013-05-13T16:01, using datafrom the Helioseismic and Magnetic Imager (HMI) of theSolar Dynamics Observatory. At least two distinct kinds ofsources appear (chromospheric and coronal) in the earlyand later phases of flare development, in addition to thewhite-light footpoint sources commonly observed in thelower atmosphere. The gradual emissions have a clearidentification with the classical loop-prominence system,with emission contributions from electron scattering andfrom the free-free continuum (as seen in soft X-rays). Thesesources may also contain other continuum and/or lineemissions and lead clearly to coronal rain in some casesobservedAuthor(s): Juan Carlos Martinez Oliveros (University of CaliforniaBerkeley), Pascal Saint-Hilaire (University of California Berkeley),Sebastien Couvidat (Stanford University), Hugh Hudson (University ofGlasgow), Sam Krucker (University of Applied Sciences North WesternSwitzerland)

123.32 – Observation of 2011-02-15 X2.2solar flare in Hard X-ray and microwavePrevious studies have shown that the energy releasemechanism of some solar flares follow the Standardmagnetic-reconnection model, but the detailed propertiesof high-energy electrons produced in the flare are still notwell understood. We conducted a unique, multi-wavelengthstudy that discloses the spatial, temporal and energydistributions of the accelerated electrons in the X2.2 solarflare on Feb. 15, 2011. We studied the source locations ofthe observed seven temporal peaks in hard X-ray (HXR)and microwave (MW) lightcurves using the Reuven RamatyHigh Energy Solar Spectroscopic Imager (RHESSI) in 50-75keV channels and Nobeyama Radioheliograph (NoRH) in 34GHz, respectively. We confirmed that peak emissions werecoming from two spatially distinct sites in HXR and MW,and in HXR we observed a sudden change between thesesites over the second and the third peak. Comparisonbetween the HXR lightcurve and the temporal variations inMW source kernel intensity also confirmed that seven peakemissions were actually coming from two sources, eachwith their own multiple peaks.Author(s): Natsuha Kuroda (New Jersey Institute of Technology),Haimin Wang (New Jersey Institute of Technology), Dale Gary (New JerseyInstitute of Technology)

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123.33 – Can return-current losses explain astrong break in RHESSI spectra?We fit the RHESSI (Ramaty High Energy Solar SpectoscopicImager) spectra from two flares with the 1D return-currentmodel in OSPEX, as well as with models containing a brokenpower law and/or a sharp, low-energy cutoff. Based onprevious studies, we know that the flattening of theseflares’ spectra is unlikely to be due to albedo ornon-uniform ionization. Both flares show compact RHESSIsources, which makes imaging spectroscopy difficult orimpossible. We verify whether the time evolution of thefitted parameters is consistent with the return-currentmodel. We look for signatures specific to return currents,such as the “bump” on higher energy non-thermal lightcurves. We also show whether the RHESSI spectra areconsistent with a 1D numerical model based on solving theenergy loss and the continuity equations for return currentand Coulomb collisions in a partially ionized atmosphere.This model is more comprehensive than the modelcurrently in OSPEX which takes into account the effect ofreturn currents in a fully ionized solar atmosphere.Author(s): Meriem Alaoui (GSFC/NASA), Gordon Holman (GSFC/NASA)

123.34 – Case Study of a Magnetic Transientin NOAA 11429 Observed by SDO/HMIDuring the M7.9 Flare on 13 March 2012NOAA 11429 was the source of an M7.9 X-ray flare at thewestern solar limb (N18° W63°) on 2012 March 13 at 17:12UT. Observations of the line-of-sight magnetic flux and theStokes I and V profiles from which it is derived were carriedout by the Solar Dynamics Observatory Helioseismic andMagnetic Imager (SDO/HMI) with a 45 s cadence over thefull disk, at a spatial sampling of 0.''5. During flare onset, atransient patch of negative flux can be observed inSDO/HMI magnetograms to rapidly appear within thepositive polarity penumbra of NOAA 11429. We presenthere a detailed study of this magnetic transient and offerinterpretations as to whether this highly debatedphenomenon represents a "real" change in the structure ofthe magnetic field at the site of the flare, or is instead aproduct of instrumental/algorithmic artifacts related toparticular SDO/HMI data reduction techniques.Author(s): Brian Harker (National Solar Observatory), Alexei Pevtsov(National Solar Observatory)

123.35 – Study of super-hot plasma in thesolar flare of August 9, 2011: Neuperteffect, acceleration of electrons and energybalance.We investigated plasma heating during the impulsive phaseof GOES X6.9 flare occurred in August 9, 2011. This event ischaracterized by large flux of soft X-ray radiation in theGOES short-wavelength channel that indicates hightemperature of emitting plasma estimated as T~33 MK.The main goal of the work is to study plasma heating andto determine role of nonthermal electrons in the energyrelease for the selected event. We analyze observationaldata of the RHESSI, GOES and SDO spacecrafts and discussspatial structure of the flare region and Neupert effect forplasmas of different temperatures. Fitting of soft X-rayspectra measured by RHESSI is made in the frame oftwo-temperature approach: emission of hot (T~20 MK) andsuper-hot (T~45 MK) plasmas. Fitting of hard X-ray spectrais made with a power-law function. To interpret the data weuse model of the flare region consisting of two separatezones with hot and super-hot temperatures, with super-hotregion being located in the highest coronal part of the flareloops where electron acceleration most probably tookplace. In the frame of the applied model the estimatedchanges of internal plasma energy and radiation heatlosses are comparable with kinetic power of nonthermalelectrons, assuming additional heat flux from the super-hotregion of the flare loops.Author(s): Ivan Sharykin (New Jersey Institute of Technology),Alexei Struminsky (Moscow Institute of Physics and Technology), IvanZimovets (Space Research Institute of RAS)

123.37 – The Compatibility of FlareTemperatures Observed with AIA, GOES,and RHESSIIn this talk we compare multi-thermal flare DEM peaktemperatures determined with SDO/AIA with thosedetermined by GOES/XRS and RHESSI using the isothermalassumption. In a set of 149 M- and X-class flares, AIA findsan average DEM peak temperature at the time of the GOESlong channel peak of 12.0±2.9 MK and Gaussian DEMwidths of log10(?T ) = 0.50±0.13. From GOES observationsof the same 149 events, a mean temperature of 15.6±2.4MK is inferred, which is higher by a factor of TGOES/TAIA =1.4±0.4. We demonstrate that this discrepancy results fromthe isothermal assumption in the inversion of the GOESfilter ratio. From isothermal fits to photon spectra atenergies of 6–12 keV of 61 of these events, RHESSI findsthe temperature to be higher (TRHESSI/TAIA = 1.9±1.0).We find that this is partly a consequence of the isothermalassumption. However, RHESSI is not sensitive to thelow-temperature range of the DEM peak, and thus onlysamples the DEM’s high-temperature tail. This is expectedto be the cause of further discrepancies. We conclude thatself-consistent flare DEM temperatures requiresimultaneous fitting of EUV and SXR fluxes.Author(s): Daniel Ryan (NASA Goddard Space Flight Center),Markus Aschwanden (Lockheed Martin Advanced Technology Cente), AidanO'Flannagain (Trinity College Dublin), Peter Gallagher (Trinity CollegeDublin)

Contributing teams: Catholic University of America

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123.38 – Energetic analysis of the whitelight emission associated to seismicallyactive flares in solar cycle 24Solar flares are explosive phenomena, thought to be drivenby magnetic free energy accumulated in the solar corona.Some flares release seismic transients, "sunquakes", intothe Sun's interior. Different mechanisms are beingconsidered to explain how sunquakes are generated. Weare conducting an analysis of white-light emissionassociated with those seismically active solar flares thathave been reported by different authors within the currentsolar cycle. Seismic diagnostics are based upon standardtime-distance techniques, including seismic holography,applied to Dopplergrams obtained by SDO/HMI and GONG.The relation between white-light emissions and seismicactivity may provide important information on impulsivechromospheric heating during flares, a prospectivecontributor to seismic transient emission, at least in someinstances. We develop a method to get an estimation ofEnergy associated whit white-light emission and comparethose results whit values of energy needed to generate asunquake according with holographic helioseismologytechniques.Author(s): Juan Camilo Buitrago-Casas (Space Sciences Lab - UCBerkeley), Juan Carlos Martinez Oliveros (Space Sciences Lab - UCBerkeley), Lindsay Glesener (Space Sciences Lab - UC Berkeley), SamKrucker (Space Sciences Lab - UC Berkeley)

123.39 – F-CHROMA. Flare Chromospheres:Observations, Models and ArchivesF-CHROMA is a collaborative project newly funded underthe EU-Framework Programme 7 "FP7-SPACE-2013-1",involving seven different European research Institutes andUniversities. The goal of F-CHROMA is to substantiallyadvance our understanding of the physics of energydissipation and radiation in the flaring solar atmosphere,with a particular focus on the flares' chromosphere. A majoroutcome of the F-CHROMA project will be the creation of anarchive of chromospheric flare observations and models tobe made available to the community for further research. Inthis poster we describe the structure and milestones of theproject, the different activities planned, as well as earlyresults. Emphasis will be given to the dissemination effortsof the project to make results of these activities available toand usable by the community.Author(s): Gianna Cauzzi (INAF), Lyndsay Fletcher (University ofGlasgow), Mihalis Mathioudakis (Queen's University Belfast), Mats Carlsson(University of Oslo), Petr Heinzel (Academy of Sciences of the CzechRepublic), Arek Berlicki (University of Wroclaw), Francesca Zuccarello(University of Catania)

123.40 – Coronal Type II Radio BurstsAssociated with Helmet Streamers andElectron Acceleration in a Streamer-ShockSystemTwo solar type II radio bursts, separated by about 24 hoursin time, are examined together. We find several commonobservational features of the two events. Firstly, bothevents are associated with coronal mass ejections (CMEs)erupting from the same active region (NOAA 11176)beneath a well-observed helmet streamer. Secondly, theradio-emitting heights obtained by fitting the type IIdynamic spectra are in agreement with those measuredfrom the CME fronts. Thirdly, the type II emissions endedonce the CME/shock fronts passed the white-light streamertip, which is presumably the magnetic cusp of the streamer.These observations lead us to propose that the closedmagnetic arcades of the streamer play an important role inelectron acceleration and type II excitation at coronalshocks. To examine such a scenario, we conduct atest-particle simulation for electron dynamics within alarge-scale partially-closed streamer magneticconfiguration swept by a coronal shock. We find thatelectrons can be trapped within the magnetic arcades andgain energy multiple times at the shock. Low energyelectrons with an initial energy of 300 eV can beaccelerated to tens of keV, energetic enough to exciteLangmuir waves and radio bursts. The results suggest thatthe scenario may be important to the generation of metrictype IIs considering the fact that most solar eruptionsoriginate from closed field regions. This scenario alsoprovides an explanation to the long-standing issue of thedisconnection between metric and interplanetary type IIbursts.Author(s): Xiangliang Kong (Shandong University, Weihai), YaoChen (Shandong University, Weihai), Fan Guo (Los Alamos NationalLaboratory), Gang Li (University of Alabama in Huntsville)

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123.41 – Towards Characterizing Early-stageSEP Fluxes with High-Cadence EUV CoronalShock ObservationsRecent advances in space-based solar observing haveenabled unprecedented access to high-cadence,high-resolution observations of the coronal dynamics. Thisis extremely important, since transient phenomena in thecorona usually cover multiple scales - from the currentspatial resolution limit in the case of reconnection, toseveral solar radii in the case of coronal waves and massejections. The latter are also thought to drive shocks in thecorona, which in turn have been shown capable ofaccelerating protons, electrons, and other species up toGeV energies in a matter of tens of minutes. These solarenergetic particles (SEPs) are a prime source of spaceweather. Historically, it has been notoriously difficult toextract information about energetic particle spectra in thecorona, due to the lack of in situ measurements. It ispossible, however, to use remote observations in order todeduce coronal shock dynamics and related particlespectra, with some reasonable assumptions. We present aneffort towards building a framework for estimating coronalSEP spectra in the early stages of real CME events, basedon a combination of fast-cadence extreme ultravioletimaging (from the SDO/AIA instrument), potential coronalmagnetic field models, and differential emission measuremodels. The ultimate goal for this framework is to givepredictions for early-stage SEP spectra for various sourcepopulations and coronal turbulence levels. It is designed ina modular fashion, and may be adapted for near real timeuse. This system can be applied for early warning andpredicting the severity of the impulsive early stages of SEPevents.Author(s): Kamen Kozarev (Harvard-Smithsonian, CfA), JohnRaymond (Harvard-Smithsonian, CfA), Michael Hammer (CornellUniversity)

123.42 – Forecast of daily solar flare peakflux using regressive and neural networkmethodsWe have developed a set of daily solar flare peak fluxforecast models using the multiple linear regression, autoregression, and artificial neural network methods. Weconsider input parameters as solar activity data fromJanuary 1996 to December 2013 such as sunspot area,X-ray flare peak flux, weighted total fluxTf=1*Fc+10*Fm+100*Fx of previous day, mean flare ratesof a given McIntosh sunspot group (Zpc), and a MountWilson magnetic classification. The hitting rate is defined asthe fraction of events whose absolute differences betweenthe observed and predicted fluxes in a logarithm scale are ?0.5. The best three input parameters related to theobserved flare peak flux are weighted total flare flux ofprevious day, Mount Wilson magnetic classification, andsunspot area. The hitting rates of flares stronger than M5class, which is regarded to be significant for space weatherforecast, are as follows: 0% for the multiple linearregression method, 30% for the auto regression method,and 69% for the neural network method. Especially, wenote that for the forecast of strong flares, the neuralnetwork method is much more effective than the othermethods.Author(s): Seulki Shin (KyungHee University), Jin-Yi Lee (KyungHeeUniversity), Yong-Jae Moon (KyungHee University)

123.43 – Rates of Large Flares in OldSolar-like Stars in Kepler Clusters NGC 6811and 6819 With Implications for the SunWe hope to better estimate the rate of very strong(Carrington event-type) flares in the Sun by studying flaresof stars in several open clusters with well determined agesusing Kepler data. Here we derive white light flaredistributions for a sample of near-solar-mass (G0-G5)dwarfs in NGC 6811 (age ~ 1 Gyr) and NGC 6819 (~ 2.5Gyr). We compare these with solar white light flare ratesand, by estimating X-ray emission from the same flaresusing a solar-based relationship, we compare the Keplerresults to other solar and stellar X-ray flare data. Weexplore implications of our results for the rates of largesolar flares. This research was supported by Kepler grantNNX13AC29G.Author(s): Steven Saar (Harvard-Smithsonian, CfA), Paul Wright(University of Southhampton), Soren Meibom (Harvard-Smithsonian, CfA),Vinay Kashyap (Harvard-Smithsonian, CfA), Jeremy Drake (Harvard-Smithsonian, CfA)

123.44 – H2 Emission in the Sun and Stars:A New Window on Spots and FlaresMolecular H2 is likely important for the formation of sunand starspots, but has been difficult to observe in the past.H2 emission has been seen in solar FUV spectra of sunspotsand flares, where it produced by fluorescent excitationdriven (primarily) by Si IV and O IV. New observations withIRIS show that the emission is strong in flares, and in loopsconnected to pores or the boundaries of umbrae. We findevidence for H2 emission in the HST spectra of severalmagnetically active, flaring, spotted stars. Once theexcitation process is better understood, observations of H2emission should permit new insight into spot formation onthe Sun and active stars.Author(s): Steven Saar (Harvard-Smithsonian, CfA), Sarah Jaeggli(Montana State Univ.)

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123.45 – Transient Small-Scale MagneticFlux Emergence and Atmospheric ResponseObserved with New Solar Telescope andSDOState-of-the art solar instrumentation is now revealing theactivity of the Sun at the highest temporal and spatialresolution. Granular-scale magnetic flux emergence and theresponse of the solar atmosphere is one of the key topics.Observations with the 1.6m aperture New Solar Telescope(NST) at Big Bear Solar Observatory (BBSO) are makingnext steps in our understanding of the solar surfacestructure. On August 7, 2013, NST observed active regionNOAA 11810 in different photospheric and chromosphericwavelengths. The region displays a group of solar pores, inthe vicinity of which we detected a site of emergingmagnetic flux accompanied by intense and very confinedabnormal granulation dynamics, observed in thephotospheric TiO 7057 A with a resolution of 0.034 “/pix.Following the expansion of exploding granules in this site,we observed a sudden appearance of an extended surge inthe HeI 10830A data (bandpass of 0.05 A). The SDO/HMIdata used to study the evolution of the magnetic field andDoppler velocities reveal a short-lived emerging loop-likestructure with strong upflows. We used the SDO/AIA data toinvestigate the response of the transition region and coronato the transient emerging flux phenomenon. We comparethe results with previous observations, and propose ascenario for the production of plasma surges by thetransient magnetic flux emergence events.Author(s): Santiago Vargas Domínguez (Big Bear SolarObservatory), Alexander Kosovichev (Stanford University)

123.46 – On Hemispheric Rule of MagneticHelicity in Solar Active RegionsThe sign of magnetic helicity in solar active regions hasbeen found to have a hemispheric preference: negative inthe northern hemisphere and positive in the southern. Thestrength of this preference reported in previous studies wasin a range of 58% -- 82%. These studies were based onexamining proxies of magnetic helicity, such as magnetictwist or current helicity density in the photosphere.Recently Liu et al. (2014) found that the strength of thehemisphere rule, tested by examining magnetic twist usingHMI vector magnetic field data, differs substantiallybetween the groups of active regions with the same sign ofmagnetic twist and writhe (56%) and with the oppositesigns (93%). They further speculated that origin ofmagnetic twist, dynamo process versus emergenceprocess, causes this difference. In this presentation, wedirectly calculate magnetic helicity in active regions, andexamine it with the hemisphere rule. This test helpsevaluate property of magnetic helicity generated by thedynamo process, and help understand intrinsic differencebetween those two groups of active regions.Author(s): Yang Liu (Stanford Univ.)

123.47 – RADMHD2S: A Global 3DRadiative-MHD Model of the UpperConvection Zone-to-Corona SystemWe present the latest results from a new, globalradiative-MHD model of the upper convection zone-to-corona system, RADMHD2S. The numerical methods buildupon those of the RADMHD model of Abbett (2007) andAbbett & Fisher (2012), and significantly extend thecapabilities of that code to allow for large-scale, sufficientlyresolved, global calculations over a non-uniform, 3Dcurvilinear (spherical) mesh. RADMHD2S utilizes ahigh-order, non-dimensionally split, semi-implicit finitevolume formalism to update the system of conservationequations in a way that properly propagates discontinuitiesin off-axis directions, while simultaneously preserving the3D solenoidal constraint on the magnetic field. In addition,we will discuss improvements in the treatment ofenergetics, radiative transport, and cross-field diffusion thatallow for more realistic data-driven modeling of the model'sphotosphere and chromosphere.Author(s): William Abbett (University of California, Berkeley),David Bercik (University of California, Berkeley)

123.48 – Active Region Lorentz Force: ACGEM Data Product Based on HMI VectorMagnetic FieldWe describe a new data product from the CGEM (CoronalGlobal Evolution Model) collaboration that estimates theLorentz force in active regions (ARs) based on HMI vectormagnetogram patches. Following Fisher et al. (2012), wecompute three components of the integrated Lorentz forceover the outer solar atmosphere every 12 minutesthroughout an AR's disk passage. These estimates,differenced during solar eruptive events, can providevaluable diagnostics on dynamic processes. We perform apreliminary survey on the major events with HMI's four-yeardata archive. We explore and characterize some of thesystematic uncertainties associated with these estimates.Author(s): Xudong Sun (Stanford University)

Contributing teams: the CGEM Team

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123.49 – Relationship between thephotospheric Poynting flux and the activeregion luminosityHow does energy radiated by active regions compare withmagnetic energy that propagates lower across thephotosphere? This is a fundamental question for energystorage and release in active regions, yet it is presentlypoorly understood. In this work we quantify and compareboth energy terms using SDO observations of the activeregion (AR) 11520. To quantify the magnetic energycrossing the photosphere, or the Poynting flux, we need toknow both the magnetic field vector B and electric fieldvector E as well. Our current electric field inversiontechnique, PDFI, combines the Poloidal-Toroidal-Decomposition method with information from Dopplermeasurements, Fourier local correlation tracking (FLCT)results, and the ideal MHD constraint, to determine theelectric field from vector magnetic field and Doppler data.We apply the PDFI method to a sequence of Helioseismicand Magnetic Imager (HMI/SDO) vector magnetogram data,to find the electric-field and hence the Poynting-fluxevolution in AR 11520. We find that most of the magneticenergy in this AR is injected in the range of $10^7$ to$10^8$ $ergs/{cm^2 s}$, with the largest fluxes reaching$10^{10}$ $ergs/{cm^2 s}$. Integrating over the activeregion this yields a total energy of order $10^{28}$ ergs/s.To quantify the active region luminosity, we use EUVVariability Experiment (EVE) and Atmospheric ImagingAssembly (AIA) spectrally resolved observations. We findthe active region luminosity of order $10^{28}$ ergs/s. Wecompare derived magnetic and radiated energy fluxes ondifferent temporal and spatial scales and estimate theiruncertainties. We also discuss the roles that potential/non-potential and emerging/shearing terms play in the totalmagnetic energy budget.Author(s): Maria Kazachenko (UC Berkeley), Richard Canfield(Montana State University), George Fisher (UC Berkeley), Hugh Hudson (UCBerkeley), Brian Welsch (UC Berkeley)

123.50 – Gravity waves in magnetized solaratmospheres from MHD simulations.The solar atmosphere is believed to be a region wheregravity waves are generated and propagate, but a varietyof effects makes observations of them rather difficult.Measurements of gravity wave properties could, however,show how they play an important role in the upperphotosphere and chromosphere and even deposit energythere. Here we show how analysis of gravity waves fromdetailed numerical simulations can be used to studymagnetic fields and energy deposition in the atmosphere,and how mode conversion to slow magneto-acoustic waveschanges their observable properties.Author(s): Jason Jackiewicz (New Mexico State University), VigeeshGangadharan (New Mexico State University)

123.51 – Understanding MeasurementsReturned by the Helioseismic and MagneticImagerThe Helioseismic and Magnetic Imager (HMI) aboard theSolar Dynamics Observatory (SDO) observes the Sun at theFeI 6173 Å line and returns full disk maps of line-of-sightobservables including the magnetic field flux, FeI line width,line depth, and continuum intensity. To properly interpretsuch data it is important to understand any issues with theHMI and the pipeline that produces these observables. Atthis aim, HMI data were analyzed at both daily intervals fora span of 3 years at disk center in the quiet Sun and hourlyintervals for a span of 200 hours around an active region.Systematic effects attributed to issues with instrumentadjustments and re-calibrations, variations in thetransmission filters and the orbital velocities of the SDOwere found while the actual physical evolutions of suchobservables were difficult to determine. Velocities andmagnetic flux measurements are less affected, as theaforementioned effects are partially compensated for bythe HMI algorithm; the other observables are insteadaffected by larger uncertainties. In order to model theseuncertainties, the HMI pipeline was tested with syntheticspectra generated through various 1D atmosphere modelswith radiative transfer code (the RH code). It was foundthat HMI estimates of line width, line depth, and continuumintensity are highly dependent on the shape of the line, andtherefore highly dependent on the line-of-sight angle andthe magnetic field associated to the model. The bestestimates are found for Quiet regions at disk center, forwhich the relative differences between theoretical and HMIalgorithm values are 6-8% for line width, 10-15% for linedepth, and 0.1-0.2% for continuum intensity. In general, therelative difference between theoretical values and HMIestimates increases toward the limb and with the increaseof the field; the HMI algorithm seems to fail in regions withfields larger than ~2000 G. This work is carried out throughthe National Solar Observatory Research Experiences forUndergraduate (REU) site program, which is co-funded bythe Department of Defense in partnership with the NSF REUProgram. The National Solar Observatory is operated by theAssociation of Universities for Research in Astronomy, Inc.(AURA) under cooperative agreement with the NationalScience Foundation.Author(s): Daniel Cohen (National Solar Observatory - SacramentoPeak), Serena Criscuoli (National Solar Observatory - Sacramento Peak)

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123.52 – Tracked Active Region Patches forMDI and HMIWe describe tracked active-region patch data products thathave been developed for HMI (HMI Active Region Patches,or HARPs) and for MDI (MDI Tracked Active Region Patches,or MDI TARPs). Both data products consist of trackedmagnetic features on the scale of solar active regions. Thenow-released HARP data product covers 2010-present(>2000 regions to date). Like the HARPs, the MDI TARP dataset is a catalog of active regions (ARs), indexed by a regionID number, analogous to a NOAA AR number, and time. TheTARPs contain 6170 regions spanning 72000 images takenover 1996-2010, and will be available in the MDI residentarchive (RA). MDI TARPs are computed based on the96-minute synoptic magnetograms and intensitygrams. Aswith the related HARP data product, the approximatethreshold for significance is 100G. Use of both image typestogether allows faculae and sunspots to be separated outas sub-classes of activity, in addition to identifying theoverall active region that they are in. After being identifiedin single images, the magnetically-active patches aregrouped and tracked from image to image. Merges amonggrowing active regions, as well as faint active regionshovering at the threshold of detection, are handledautomatically. Regions are tracked from their inception untilthey decay within view, or transit off the visible disk. Foreach active region and for each time, a bitmap image isstored containing the precise outline of the active region.Also, metadata such as areas and integrated fluxes arestored for each AR and for each time. Because there is across-calibration between the HMI and MDI magnetograms(Liu et al. 2012), it is straightforward to use the sameclassification and tracking rules for the HMI HARPs and theMDI TARPs. We show results demonstrating regioncorrespondence, region boundary agreement, andagreement of flux metadata using the approximately 140regions in the May 2010-October 2010 time period. Weenvision several uses for these data products, includingdata subsetting and per-active-region studies such as therelation between AR structure and energetic events likeflares. Also, the combined HARP/MDI-TARP catalog canenable extended studies, such as solar irradiance, acrosscycles 23 and 24, and allow analyses that had beenconfined to just a handful of ARs to be extended to a largerset.Author(s): Michael Turmon (JPL/Caltech), J. Todd Hoeksema (StanfordUniv.), Monica Bobra (Stanford Univ.)

123.54 – A New Ground-Based Network forSynoptic Solar Observations: The SolarPhysics Research Integrated Network Group(SPRING)SPRING is a project to develop a geographically distributednetwork of instrumentation to obtain synoptic solarobservations. Building on the demonstrated success ofnetworks to provide nearly-continuous long-term data forhelioseismology, SPRING will provide data for a wide rangeof solar research areas. Scientific objectives include internalsolar dynamics and structure; wave transport in the solaratmosphere; the evolution of the magnetic field over theactivity cycle; irradiance fluctuations; and space weatherorigins. Anticipated data products include simultaneousfull-disk multi-wavelength Doppler and vector magneticfield images; filtergrams in H-Alpha, CaK, and white light;and PSPT-type irradiance support. The data will be obtainedwith a duty cycle of around 90% and at a cadence noslower than one minute. The current concept is a multi-instrument platform installed in at least six locations, andwhich will also provide context information for large-aperture solar telescopes such as EST and the DKIST. Thereis wide support for the idea within the EU and the US solarresearch communities. The project is in the early planningstages, and we are open to and looking for participants inthe science and instrument definition.Author(s): Frank Hill (National Solar Obs.), Markus Roth(Kiepenheuer-Institut für Sonnenphysik), Michael Thompson (NCAR),Sanjay Gusain (Kiepenheuer-Institut für Sonnenphysik)

123.55 – An Improved PeriodogramTechnique for 2-D PSF EqualizationThe Multi-Order Extreme Ultraviolet Spectrograph (MOSES)forms images of the transition region at HE II 30.4 in threespectral orders. Subtle differences between these imagesencode line profile information. However, differences ininstrument point-spread function (PSF) in the three orderslead to non-negligible systematic errors in the retrieval ofthe line profiles. We describe an improved periodogramtechnique for equalizing the PSFs, and provide numericalverification of the technique's validity.Author(s): Shane Atwood (Montana State University), CharlesKankelborg (Montana State University)

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123.56 – An Airborne Infrared Telescope andSpectrograph for Solar Eclipse ObservationsThe solar infrared spectrum offers great possibilities fordirect spatially resolved measurements of the solar coronalmagnetic fields, via imaging of the plasma that isconstrained to follow the magnetic field direction and viaspectro-polarimetry that permits measurement of the fieldstrength in the corona. Energy stored in coronal magneticfields is released in flares and coronal mass ejections (CME)and provides the ultimate source of energy for spaceweather. The large scale structure of the coronal field, andthe opening up of the field in a transition zone between theclosed and open corona determines the speed andstructure of the solar wind, providing the backgroundenvironment through which CMEs propagate. At present ouronly direct measurements of the solar magnetic fields arein the photosphere and chromosphere. The ability todetermine where and why the corona transitions fromclosed to open, combined with measurements of the fieldstrength via infrared coronal spectro-polarimetry will giveus a powerful new tool in our quest to develop the nextgeneration of forecasting models. We describe a first stepin achieving this goal: a proposal for a new IR telescope,image stabilization system, and spectrometer, for the NCARHIPER GV aircraft. The telescope/spectrograph will operatein the 2-6micron wavelength region, during solar eclipses,starting with the trans-north American eclipse in August2017. The HIAPER aircraft flying at ~35,000 ft will providean excellent platform for IR observations. Our imaging andspectroscopy experiment will show the distribution andintensity of IR forbidden lines in the solar corona.Author(s): Edward DeLuca (Harvard-Smithsonian, CfA), PeterCheimets (Harvard-Smithsonian, CfA), Leon Golub (Harvard-Smithsonian,CfA)

123.57 – Performance Measurements of anIntensified APS Detector for SPICE on SolarOrbiterThe Spectral Imaging of the Coronal Environment (SPICE)instrument for the Solar Orbiter mission will makespectroscopic observations of the Sun's low corona tocharacterize the plasma properties of the source regions ofthe solar wind. The detector package for SPICE, provided bythe NASA Goddard Space FLight Center, consists of twomicrochannel-plate (MCP) intensified Active Pixel Sensor(APS) detectors covering the short (702-792 Angstroms)and long (972-1050 Angstroms) wavelength bandpasses.The long wavelength detector will also provide coverage insecond order between 485-525 Angstroms. We report hereon measurements made on the engineering model of theSPICE detector in a vacuum tank facility at the RutherfordAppleton Laboratory in Harwell, UK. These measurementsinclude the detector flat field, sensitivity, resolution,linearity, and statistical noise. A krypton resonance lampoperating at 1236 Angstroms was used to stimulate thedetector. Results at this wavelength are combined with thequantum efficiency measurements of the individual MCPs atthis and other wavelengths covering the entire wavelengthrange to provide a complete calibration curve for theinstrument. A calibrated NIST photodiode was used todetermine the absolute brightness of the lamp.Author(s): William Thompson (NASA/GSFC), Joseph Davila(NASA/GSFC), Gregory Woytko (NASA/GSFC), Thomas Devlin (NASA/GSFC),Patrick Jordan (NASA/GSFC), Alberto Rosanova (NASA/GSFC), WilliamChang (NASA/GSFC), Nelson Reginald (NASA/GSFC), Thomas Plummer(NASA/GSFC), Patrick Haas (NASA/GSFC), Martin Caldwell (RutherfordAppleton Laboratory), Mark Anderson (Rutherford Appleton Laboratory),Paul Eccleston (Rutherford Appleton Laboratory), Douglas Griffin(Rutherford Appleton Laboratory), Oswald Siegmund (Sensor Sciences,LLC)

123.58 – Tools for 3D Spectropolarimetry - ABirefringent Fiber Optic Image SlicerImage-slicing technology benefits astronomicalspectropolarimetry by transposing a three-dimensionalinformational set--two spatial and one spectraldimension--into a format more amenable to simultaneouscoverage by conventional spectrographs. To probe, forexample, the magnetism of the fine-scaled, dynamicchromosphere, methods beyond slit-basedspectropolarimetry are essential. Fiber optic integral fieldunits (IFUs) present one promising solution. The importanceof a birefringent fiber-optic IFU design stems from the needof spatio-temporal modulation to correct for spuriouspolarization signals induced either by platform jitter oratmospheric seeing. Standard stock fibers do not typicallypreserve polarization. Here we characterize the polarizationresponse of a close-packed IFU based on rectangular opticalfibers, currently under development for the Diffraction-Limited Near-IR Spectropolarimeter, a facility instrument ofthe Advanced Technology Solar Telescope. Solarobservations utilizing this device will be presented.Author(s): Thomas Schad (University of Hawaii), Haosheng Lin(University of Hawaii)

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123.59 – Slitless Solar SpectroscopySpectrographs have traditionally suffered from the inabilityto obtain line intensities, widths, and Doppler shifts overlarge spatial regions of the Sun quickly because of theirnarrow instantaneous field of view. This has limited thespectroscopic analysis of rapidly varying solar features like,flares, CME eruptions, coronal jets, and reconnectionregions. Imagers, on the other hand, have provided hightime resolution images of the full Sun with limited spectralresolution. In this paper we present recent advances indeconvolving spectrally dispersed images obtained throughbroad slits. We use this new theoretical formulation toexamine the effectiveness of various potential observingscenarios, spatial and spectral resolutions, signal to noiseratio, and other instrument characteristics. We test thismethod on two specific observing scenarios. With theoriginal method developed for the single spectral line case,we first analyze the effect of overlapping spectral lines onthe resulting spectral parameters. Second, we determinehow well the method performs when given dispersed imageinput with either three orders (0, +1, -1), or with two orders(0, +1). In both cases a more accurate Gauss error functioncalculation is employed on the dispersed images. Thisinformation will lay the foundation for a new generation ofspectral imagers optimized for slitless spectral operation,enabling us to obtain spectral information in transient solarevents.Author(s): John O'Neill (Catholic University of America), JosephDavila (Goddard Space Flight Center), Figen Oktem (University of Illinois atUrbana-Champaign)

123.60 – The Expanded Owens Valley SolarArray (EOVSA)The Expanded Owens Valley Solar Array (EOVSA) near BigPine, CA is undergoing commissioning as a solar-dedicatedmicrowave imaging array operating in the frequency range2.5-18 GHz. The solar science to be addressed focuses onthe 3D structure of the solar corona (magnetic field,temperature and density), and on the particle acceleration,transport and heating in solar flares. The project willsupport the scientific community by providing open dataaccess and software tools for analysis and modeling of thedata, to exploit synergies with on-going solar research inother wavelengths. The array consists of a total of 15antennas, including the two 27-m antennas with He-cooledreceivers for sensitive calibration, and thirteen 2.1-mantennas that each view the entire disk of the Sun. Thesystem includes a completely new control system,broadband signal transmission, and high-speed digitalsignal processing, using new technology developed for theFrequency Agile Solar Radiotelescope (FASR). We presentan overview of the instrument, the current status ofcommissioning activities, and some initial observations toassess performance. This research is supported by NSFgrants AST-1312802, and NASA grants NNX11AB49G andNNX10AF27G to New Jersey Institute of Technology.Author(s): Dale Gary (NJIT), Gordon Hurford (UC/Berkeley), Gelu Nita(NJIT), Stephen White (AFRL), James McTiernan (UC/Berkeley), GregoryFleishman (NJIT)

123.61 – Flight Performance of the HEROESSolar Aspect SystemHard X-ray (HXR) observations of solar flares reveal thesignatures of energetic electrons, and HXR images withhigh dynamic range and high sensitivity can distinguishbetween where electrons are accelerated and where theystop. Furthermore, high-sensitivity HXR measurements maybe able to detect the presence of electron acceleration inthe non-flaring corona. The High Energy Replicated Opticsto Explore the Sun (HEROES) balloon mission added thecapability of solar observations to an existing astrophysicsballoon payload, HERO, which used grazing-incidenceoptics for direct HXR imaging. The HEROES Solar AspectSystem (SAS) was developed and built to provide pointingknowledge during solar observations to better than the ~20arcsec FWHM angular resolution of the HXR instrument. TheSAS consists of two separate systems: the Pitch-Yaw aspectSystem (PYAS) and the Roll Aspect System (RAS). The PYAScompares the position of an optical image of the Sunrelative to precise fiducials to determine the pitch and yawpointing offsets from the desired solar target. The RASimages the Earth's horizon in opposite directionssimultaneously to determine the roll of the gondola.HEROES launched in September 2013 from Fort Sumner,New Mexico, and had a successful one-day flight. Wepresent the detailed analysis of the performance of the SASfor that flight.Author(s): Albert Shih (NASA/GSFC), Steven Christe (NASA/GSFC),Marcello Rodriguez (NASA/GSFC), Kyle Gregory (NASA/GSFC), AlexanderCramer (NASA/GSFC), Melissa Edgerton (NASA/GSFC), Jessica Gaskin(NASA/MSFC), Brian O'Connor (NASA/MSFC), Alexander Sobey(NASA/MSFC)

123.62 – Observing the Sun in hard X-raysusing grazing incidence optics: the FOXSIand HEROES projectsSolar flares accelerate particles up to high energies throughvarious acceleration mechanisms which are not currentlyunderstood. Hard X-rays are the most direct diagnostic offlare-accelerated electrons. However past and current hardx-ray observation lack the sensitivity and dynamic rangenecessary to observe the faint signature of acceleratedelectrons in the acceleration region, the solar corona. Theselimitations can be easily overcome through the use of HXRfocusing optics coupled with solid state pixelated detectors.We present results from the recent flights of two sub-orbitalpayloads that have applied grazing incidence HXR optics tosolar observations. FOXSI, short for Focusing Optics X-RaySolar Imager, was launched on a sounding rocket inNovember 2012 from White Sanda and observed a solarflare. HEROES, short for High Energy Replicated Optics toExplore the Sun, observed the sun for 7 hours from a highaltitude balloon on September 21, 2013. We present recentresults as well as the capabilities of a possible futuresatellite missionAuthor(s): Steven Christe (NASA GSFC), Lindsay Glesener (Universityof California, Berkeley), Sam Krucker (Facchoschule Nordwestschweiz),Albert Shih (NASA GSFC), Jessica Gaskin (NASA MSFC), Colleen Wilson(NASA MSFC)

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123.63 – The SUVIT Instrument on theSolar-C MissionSolar-C is a new space mission being proposed to JAXA, withsignificant contributions anticipated from NASA, ESA, andEU countries. The main scientific objectives are to: revealthe mechanisms for heating and dynamics of thechromosphere and corona and acceleration of the solarwind; determine the physical origin of the large-scaleexplosions and eruptions that drive short-term solar,heliospheric, and geospace variability; use the solaratmosphere as a laboratory for understanding fundamentalphysical processes; make unprecedented observations ofthe polar magnetic fields. The unique approaches of Solar-Cto achieve these goals are to: determine the properties andevolution of the 3-dimensional magnetic field, especially onsmall spatial scales, and for the first time observed in thecrucial low beta plasma region; observe all the temperatureregimes of the atmosphere seamlessly at the highestspatial resolution ever achieved; observe at high cadencethe prevailing dynamics in all regions of the atmosphere;determine physical properties from high resolutionspectroscopic measurements throughout the atmosphereand into the solar wind. The powerful suite of instrumentsonboard Solar-C will be sensitive to temperatures from thephotosphere (~5500 K) to solar flares (~20 MK) with notemperature gap, with spatial resolution at all temperaturesof 0.3? or less (0.1? in the lower atmosphere) and at highcadence. The purpose of the Solar UV-Visible-IR Telescope(SUVIT) is to obtain chromospheric velocity, temperature,density and magnetic field diagnostics over as wide a rangeof heights as possible, through high cadence spectral lineprofiles and vector spectro-polarimetry. SUVIT is ameter-class telescope currently under study at 1.4m inorder to obtain sufficient resolution and S/N. SUVIT has twocomplementary focal plane packages, the Filtergraph thatmakes high cadence imaging observations with the highestspatial resolution and the Spectro-polarimeter that makesprecise spectro-polarimetric observations. With theirpowerful sets of spectral lines, FG and SP collect physical

measurements from the lower photosphere to upperchromosphere with much better spatial and temporalresolution than Hinode SOT.Author(s): Theodore Tarbell (LMSAL), Kiyoshi Ichimoto (KyotoUniversity)

123.64 – Current and future solarobservation using focusing hard X-rayimagersThe efficient processes that accelerate particles in solarflares are not currently understood. Hard X-rays (HXRs) areone of the best diagnostics of flare-accelerated electrons,and therefore of acceleration processes. Past and currentsolar HXR observers rely on indirect Fourier imaging andthus lack the necessary sensitivity and imaging dynamicrange to make detailed studies of faint HXR sources in thesolar corona (where particle acceleration is thought tooccur). A future generation of solar HXR observers willinstead likely rely on direct HXR focusing, which canprovide far superior sensitivity and imaging dynamic range.The first wave of focused solar HXR studies is alreadyunderway, including sounding rocket and high-altitudeballoon payloads, and, in the near future, solar observationby the NuSTAR astrophysics observatory. This poster will (1)summarize the capabilities of current solar HXRinstruments, comparing the science that can be done fromeach platform, and (2) discuss the scientific power of afuture, dedicated, spaceborne observatory optimized toobserve HXRs from the Sun.Author(s): Lindsay Glesener (University of California, Berkeley),Amir Caspi (University of Colorado, Boulder), Steven Christe (GoddardSpace Flight Center), Iain Hannah (University of Glasgow), Hugh Hudson(University of California, Berkeley), Gordon Hurford (University of AppliedSciences Northwestern Switzerland), Brian Grefenstette (CaliforniaInstitute of Technology), Sam Krucker (University of Applied SciencesNorthwestern Switzerland), Andrew Marsh (University of California, SantaCruz), Richard Mewaldt (California Institute of Technology), MichaelPivovaroff (Lawrence Livermore National Laboratory), Albert Shih (GoddardSpace Flight Center), David Smith (University of California, Santa Cruz),Julia Vogel (Lawrence Livermore National Laboratory), Stephen White (AirForce Research Laboratory)

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102 – Extrasolar Planets: Characterization and TheoryOral Session – America Ballroom North/Central – 02 Jun 2014 10:00 AM to 11:30 AMChair(s):Sarah Ballard (Harvard University)

102.01 – Influence of UV activity on theSpectral Fingerprints of Earth-like Planetsaround M dwarfsA wide range of potentially rocky transiting planets in thehabitable zone (HZ) have been detected by Kepler as wellas ground-based searches. The spectral type of the hoststar will influence our ability to detect atmospheric featureswith future space and ground based missions like JWST,GMT and E-ELT. Particularly the active and inactive M starsare a stellar class, covering a wide range of UV luminosity,that will influence the detectability of habitable conditions.The UV emission from a planet's host star dominates thephotochemistry and thus the resultant observable spectralfeatures. Using the latest UV spectra obtained by Hubble aswell as IUE, we model Earth-like planets orbiting a widerange of M-dwarfs from M0 to M9 for both active andinactive stars. These planets are the first ones that shouldbecome available to observations with JWST and E-ELT. Awide range of such targets will soon be identified in ourSolar Neighborhood by the 2017 TESS mission.Author(s): Sarah Rugheimer (Harvard University - CFA), LisaKaltenegger (MPIA), Antigona Segura (Universidad Nacional Autónoma deMéxico), Jeffrey Linsky (University of Colorado - Boulder, JILA), SubhanjoyMohanty (Imperial College London)

102.02 – Effect of Exoplanet Clouds onVisible Wavelength Albedo Spectra andPhase CurvesWe use a planetary albedo model to investigate variationsin visible wavelength phase curves of the exoplanetKepler-7b and a theoretical Jupiter-like exoplanet at 2 AU.Thermal and cloud properties for these exoplanets arederived using one-dimensional radiative-convective andcloud simulations. The presence of clouds on theseexoplanets significantly alters their planetary albedospectra. We show that non-uniform cloud coverage on thedayside of tidally locked exoplanets will manifest aschanges to the magnitude and shift of the phase curve. Weinvestigate a test case of our model using a Jupiter-likeplanet orbiting at 2.0 AU from a solar type star to considerthe effect of H2O clouds. The model is then extended to theexoplanet Kepler-7b and considers the effect of Mg2SiO4clouds. We show that, depending on the observationalfilter, the shift of the phase curve maximum will be ~2-10°for a Jupiter-like planet and up to ~30° ( ~0.08 in orbitalphase) for hot Jupiter exoplanets at visible wavelengths.The model presented in this work can be adapted for avariety of planetary cases at visible wavelengths to includevariations in planet-star separation, gravity, metallicity, andsource-observer geometry. Finally, we tailor our model forcomparison with the recent optical phase-curveobservations of Kepler-7b with the Kepler space telescope.We show that models where Kepler-7b has slightly morethan half of its dayside covered in Mg2SiO4 clouds providea good fit to the observed phase-curve magnitude andoffset. We also investigate the effect of varying particlesizes and sedimentation efficiencies to explore the rangesthat do not fit the currently available data for Kepler-7b andHD189733b. Furthermore; we explore the use of 3Dtemperature maps/models to more accurately portray thevarying albedo across the planet.Author(s): Matthew Webber (MIT), Nikole Lewis (MIT), Mark Marley(NASA Ames Research Center), Jonathan Fortney (University of California),Kerri Cahoy (MIT)

102.04 – HARPS-N Contributions to theMass-Radius Diagram for Rocky ExoplanetsScience operations began with HARPS-N on the TNG inAugust 2012. About half of the 80 nights per year allocatedto the HARPS-N Collaboration have been dedicated tofollow-up observations of bright Kepler Objects of Interestthat showed promise of being rocky. In this presentation weshow how mass determinations from HARPS-N areimproving our understanding of the mass-radius diagramfor rocky exoplanets, including recent results for Kepler 78and Kepler 10.Author(s): David Latham (Harvard-Smithsonian, CfA), DimitarSasselov (Harvard-Smithsonian, CfA)

Contributing teams: HARPS-N Collaboration

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102.05 – Three Distinct Exoplanet RegimesInferred From Host Star MetallicitiesThe occurrence rate of exoplanets smaller than 4 Earthradii (RE) in short orbits is ~50%. Despite their sheerabundance, the compositions of planets populating thisregime are largely unknown. The available evidencesuggests the existence of a compositional range, fromsmall high-density rocky planets to low-density planetsconsisting of rocky cores surrounded by thick H/He gasenvelopes. Understanding the transition from the gaseousplanets to Earth-like rocky worlds is important to estimatethe number of potentially habitable planets in our Galaxyand provide constraints on planet formation theories. Here,we report the abundances of heavy elements (metallicities)of over 400 stars hosting 600 exoplanet candidatesdiscovered by the Kepler Mission and find that theexoplanets can be categorized into three populationsdefined by statistically distinct (~ 4.5?) metallicity regions.We interpret these regions as reflecting the formationregimes of terrestrial-like planets (RP < 1.7 RE), gas-dwarfplanets with rocky cores and H/He envelopes (1.7 < RP <3.9 RE) and ice/gas-giant planets (RP > 3.9 RE). Thesetransitions resonate well with those inferred fromdynamical mass estimates, implying that host-starmetallicity – a proxy for the initial solid inventory of theprotoplanetary disk – is a key ingredient regulating thestructure of planetary systems.Author(s): Lars Buchhave (Centre for Star and Planet Formation),Martin Bizzarro (Centre for Star and Planet Formation), David Latham(Harvard-Smithsonian Center for Astrophysics), Dimitar Sasselov (Harvard-Smithsonian Center for Astrophysics)

102.06 – Detailed Abundances of a Planet-Hosting Wide Binary System: Did PlanetFormation Imprint Chemical Signatures inthe Atmospheres of HD20782/81?We present a detailed chemical abundance analysis of aplanet-hosting wide binary system (HD20782 + HD20781),where both stars are G-dwarfs, and each of them hostsgiant planets on eccentric orbits with pericenters ~< 0.2AU. We investigate if giant planets on such orbits couldscatter inner rocky planets into the atmospheres of theirhost stars, and thereby imprint a detectable chemicalsignature in the stellar photospheric abundances. Usinghigh-resolution, high signal-to-noise echelle spectra, wederive the abundances of 15 elements. In addition, therefractory elements (Tc > 900 K) in both stars show apositive correlation between the elemental abundances andcondensation temperatures (Tc), with similar slopes of

~1×10-4 dex K-1. In each star, the measured positive

correlations are imperfect, with a scatter of ~5×10-5 dex

K-1 about the mean trend; also, certain elements (Na, Al,Sc) are similarly deviant in both stars. We interpret theseresults in the context of simulations of giant planetmigration that predict the accretion of H-depleted rockymaterial by the host star. We demonstrate that a simplemodel for a solar-type star accreting material withEarth-like composition predicts a positive -- but imperfect --correlation between [X/H] and Tc. According to this model,our measured slopes are consistent with the ingestion of10-20 Earths by both HD20782 and HD20781.Author(s): Claude Mack (Vanderbilt University), Keivan Stassun(Vanderbilt University), Simon Schuler (University of Tampa), John Norris(The Australian National University)

102.07 – Dating Red Dwarfs: Determiningthe Ages of Red Dwarf Stars and theirHosted PlanetsRed Dwarf (dwarf M=dM) stars comprise over 75% of thestars in the Galaxy. The recent statistical analysis ofexoplanet systems from the Kepler Mission indicates thatabout 15% of red dwarf stars host Earth-size planetsorbiting in the liquid water Habitable Zones (HZ) of theirhost stars. This indicates that within 10 pc (~33 Ly) of theSun (which contains ~240 dM stars), there should be about35 potentially habitable Earth-size planets. Extrapolating tothe entire Galaxy indicates that about 50-100 billionearth-size planets may be orbiting within the HZs of reddwarfs. Determining the ages and radiation/plasmaproperties of these planet hosting dM stars is crucial inassessing the potential for life on their HZ exoplanets. Withthese aims in mind we have been carrying out multi-wavelength (X-ray - IR) studies of dM stars as part of ourNSF/NASA sponsored “Living with a Red Dwarf” Program.Due to their low masses, nuclear evolution of red dwarfs isvery slow and their physical properties (e.g. L/Lo, Teff, R/Ro)do not significantly change over the age of the universeThis makes it nearly impossible to determine (nuclear)evolutionary ages as is done with more massive stars.However, their rotation-related magnetic dynamoproperties such as- coronal X-ray and chromosphericemissions and star spots coverage dramatically decreasewith time as the stars spin down from angular momentumloss via magnetic winds We report on the ongoingcalibration of Age-Rotation and (magnetic) Activity relationsof dM stars. The ages of the calibrator stars are found frommemberships in clusters, & moving groups as well asmemberships in wide binaries - ages known from whitedwarf & main sequence star components. Kinematical agesare used for old high velocity stars. Using these relations,the ages of a dM stars can be estimated from theirmeasured rotation periods, and/or from coronal &chromospheric emissions. We apply these relations todetermine ages of nearby dM stars that host potentiallyhabitable planets that include: GJ 581, GJ 667C, HD 85572,and HD 40307. We acknowledge the support from NSF/RUIgrant AST-1009903, and NASA/CHANDRA GO1-12024X,GO2-13020X and HST-GO-13020.01-AAuthor(s): Edward Guinan (Villanova Univ.), Scott Engle (VillanovaUniv.), Evan Kullberg (Villanova Univ.), William Watson (Villanova Univ.),Scott Michener (Villanova Univ.)

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102.08 – Kepler 56: Present and FutureConfiguration and ObliquityKepler-56 is an interesting multi-planet system with twocoplanar inner planets that are highly misaligned with theirparent star, and accompanied by an outer 3.3 Jupiter massplanet with an unknown inclination. Determining the truespin orbit angle and the inclination of the outer companionis valuable to study the physical processes that canproduce the misalignment. Here, using the observed line ofsight measurements, we can constrain the true spin orbitangle and the inclination of the outer companion. Thesedepend on the initial configuration of the system. Weconsider two inherent scenarios: the first scenario assumesthe stellar spin axis to be initially aligned with the inner twoplanets' angular momentum, and it favors a large range ofmutual inclination (~20 -160 degree) between the innerplanets and the outer companion. Tighter constraints canbe achieved if the true spin orbit angle can be measured(from both asteroseismology and Rossiter-McLaughlinmeasurements). The second scenario assumes the stellarspin axis to be aligned with the total angular momentum ofthe system, and it favors the mutual inclination to bearound ~40 or ~130 degree. Future observation of themutual inclination may distinguish the two scenarios anduncover the formation processes of this system. In addition,by modeling the stellar evolution and its tidal effects on thesystem, we predict that the innermost planet will beengulfed within ~130 Myr.

Author(s): Gongjie Li (Harvard Univ.), Smadar Naoz (Harvard Univ.),Francesca Valsecchi (Center for Interdisciplinary Exploration and Researchin Astrophysics (CIERA), Northwestern University), John Johnson (HarvardUniv.), Frederic Rasio (Department of Physics and Astronomy,Northwestern University)

102.09 – Planets in Wide Binaries fromKepler: Ages, Stability and Evolution ofPlanetary SystemsUsing the Kepler Input Catalog and the fourth U.S. NavalObservatory CCD Astrograph Catalog, we have identified1509 common proper motion (CPM) binaries in the Keplerfield of view, of which a small subset host planetcandidates, or Kepler Objects of Interest (KOIs). We haveverified the fidelity of the CPM pairs using a Galactic modeland follow-up astrometric observations. We present 73 KOIsdistributed over 58 CPM pairs and highlight the first widebinary system (separation > 1000 AU) where both stellarcomponents host at least one KOI. Because our binarysample was initially targeted for a gyrochronology analysis,we also present measurements of stellar rotation periodsand preliminary estimates of stellar (and planetary) ages.We use these extrapolated planetary ages to investigatelongterm planet stability in wide binaries and test potentialformation and evolution scenarios of these dynamicallycomplex systems.Author(s): Kolby Weisenburger (Boston University), Andrew West(Boston University), Kenneth Janes (Boston University), Saurav Dhital(Embry-Riddle Aeronautical University)

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103 – Solar Magnetism IMeeting-in-a-Meeting – America Ballroom South – 02 Jun 2014 10:00 AM to 11:30 AMChair(s):Amy Winebarger (NASA Marshall Space Flight Center)

103.01D – Characterizing and ModelingMagnetic Flux Transport in the Sun’sPhotosphere and Determining Its Impact onthe Sunspot CycleCharacterization and modeling magnetic flux transportwithin the surface layers of the Sun are vital to explainingthe 11 year sunspot cycle. I have characterized thedifferential rotation (DR) and meridional flow (MF) and theirvariations since 1996 using a cross-correlation technique onmagnetograms (maps of the magnetic field at the surfaceof the Sun). The MF is faster at solar cycle minimum andslower at maximum. Furthermore, the MF speeds thatpreceded the Solar Cycle 23/24 minimum were ~20% fasterthan the MF speeds that preceded the prior minimum. Thisfaster MF has been suggested to have caused weaker polarfield strengths and thus the subsequent extended solarminimum and an unusually weak cycle 24. I have modeledsurface magnetic flux transport with a model that advectsthe magnetic flux emerging in sunspots using thenear-surface flows. These flows include the axisymmetricDR and MF and the non-axisymmetric cellular convectiveflows (supergranules), all of which vary in time as indicatedby direct observations. At each time step, magnetic mapsof the entire Sun are created. I have tested thepredictability of this model using daily sunspot area data assources of new magnetic flux. I found that the evolution ofthe polar fields can be reliably predicted many years inadvance. The model was then used to determine theimpact of MF variations on the sunspot cycle. Onesimulation included a MF that is constant, a secondincluded a MF that has the observed variations in time, anda third included a MF in which the observed variations wereexaggerated. The simulations show that the variations inthe MF over cycle 23 produce polar fields that are ~20%stronger, rather than weaker. This suggests that the causeof the weak polar fields at the end of Cycle 23 should beattributed to the emergence of fewer active region sources,rather that the variation in the meridional flow.Author(s): Lisa Upton (University of Alabama Huntsville), DavidHathaway (NASA/MSFC)

103.02 – Subsurface Structure of ActiveRegionsMagneto-convection simulations with horizontal, untwistedmagnetic field advected into the domain at large (20Mm)depth spontaneously form magnetic loops which emerge asactive regions. An active regions emerges as a fragmented,braided magnetic loop. This is what makes the magneticflux first appear with mixed polarities, that then counterstream into the leading and following spots at the loop legs.After emergence, braided vertical legs are left behind whichextend to large depths in the convection zone at the downflow boundaries of the large underlying convective cells.Movies of the emergence process and the subsurfacestructure underneath the active region will be presented.Author(s): Robert Stein (Michigan State Univ.), Aake Nordlund(Copenhagen University)

103.03 – Validation Tests of Data DrivenMagnetic Flux EmergenceThe emergence of magnetic flux through the solarphotosphere into the corona is a key problem tounderstanding the energization of the solar corona. Withthe advent of high spatial and temporal resolution solarvector magnetic field measurements, it may now bepossible to simulate the dynamical evolution of the coronaby using these measurements as the driving boundarycondition for magnetohydrodynamical (MHD) simulations ofthe corona. First, however, methods for using this data todrive simulations must be validated via quantitative tests.We report here on a series of such tests wherein the drivinginputs are taken from self-consistent simulations of theemergence of flux ropes from the upper convection zonethrough the photosphere and chromosphere into the lowcorona. Photospheric MHD output from these simulations isthen used to drive new simulations, and the driven resultsare compared against the original results for a variety ofdriving assumptions and algorithms. We will focus here onthe relative advantages and disadvantages of data drivinga higher order finite-element-based MHD code (HiFi) versusdata driving a lower order Lagrangian remap-based MHDcode (LARE3D). For each code, we will report on thenecessary input conditions (spatial and temporal resolution,specification of MHD variables, and specification of verticalgradients) needed to reproduce a high level of agreementbetween the original and the driven simulations. Finally, wewill report on the level of agreement achieved when usingdriving input equivalent to that of current solarobservations. Based on these tests, we will address theprospects for using high time and spatial resolution vectormagnetogram observations to drive MHD simulations of thesolar chromosphere and corona. This work was supportedby the ONR 6.1 and the NASA LWS programs.Author(s): Mark Linton (Naval Research Laboratory), VyacheslavLukin (Naval Research Laboratory), James Leake (George MasonUniversity), Peter Schuck (NASA Goddard Space Flight Center)

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103.04 – Multiscale Properties of the LocalDynamo on the SunDynamics of the quiet Sun represents a background ('salt-and-pepper') state for powerful manifestations of solaractivity. Current numerical simulations have shown thatsmall-scale turbulent dynamics can strongly couple withprocesses on larger scales, such as formation of pores andsunspots. We perform 3D MHD radiative simulations of toplayers of the convection zone and the low atmosphere,taking into account effects of turbulence, magnetic fields,ionization and excitation of all abundant elements. Tomodel the dynamo process we carry a series of thesimulations with various initial weak levels of magnetic fieldperturbations. The results show that an initial, randomlydistributed ('seed') magnetic field of 1 micro-gauss, greatlyamplifies by subsurface turbulent dynamics. The selfgenerated magnetic field (dynamo) reaches 2 kG magneticlevels in the photosphere. The local dynamo processprimary operates 1 Mm below the surface where themagnetic fields are amplified by helical flows. Thesedynamo-generated magnetic fields are transported bydownflows into deeper layers. The process of the magneticfield amplification has a substantially multiscale character,during which self-organized turbulent helical flows workcoherently on scales much larger then the turbulent scales.We discuss the apparent contradiction of our results withcurrent paradigm that local dynamo can generate magneticfields only on the small turbulent scales. We compare ourresults with other simulations and observations.Author(s): Irina Kitiashvili (Stanford University), AlexanderKosovichev (Stanford University), Nagi Mansour (NASA Ames ResearchCenter), Alan Wray (NASA Ames Research Center)

103.05 – The Photospheric Poynting Fluxand Coronal HeatingSome models of coronal heating suppose that random (cf.,coherent) convective motions at the photosphere shufflethe footpoints of coronal magnetic fields and thereby injectsufficient magnetic energy upward to account for observedcoronal and chromospheric energy losses in active regions.Using high-resolution observations of plage magnetic fieldsmade with the Solar Optical Telescope aboard the Hinodesatellite, we observationally test this idea by estimating theupward transport of magnetic energy --- the verticalPoynting flux, S_z --- across the photosphere in a plageregion. To do so, we combine: (i) estimates of photospherichorizontal velocities, v_h, determined by local correlationtracking applied to a sequence of line-of-sight magneticfield maps from the Narrowband Filter Imager, with (ii) avector magnetic field measurement from theSpectroPolarimeter. Plage fields are ideal observationaltargets for estimating energy injection by convection,because they are: (i) strong enough to be measured withrelatively small uncertainties; (ii) not so strong thatconvection is heavily suppressed (as within umbrae); and(iii) unipolar, so S_z in plage is not influenced by mixed-polarity processes (e.g., flux emergence) that cannotexplain steady heating in stable, active-region fields. In thisand a previously analyzed plage region, we found that theaverage S_z varied between the regions, but was positive(upward) and sufficient to explain coronal heating, withvalues near 2 x 10^7 erg/ cm^2/ s. We find the energyinput per unit magnetic flux to be on the order of a fewtimes 10^4 erg/ s/ Mx. A comparison of intensity in a Ca IIimage co-registered with one plage magnetogram showsstronger spatial correlation with unsigned vertical field,|B_z|, than either S_z or horizontal flux density, |B_h|.Author(s): Brian Welsch (UC-Berkeley)

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103.06 – Polarity Reversal of the SolarPhotospheric Magnetic Field During ActivityCycle 24The large-scale solar magnetic field reverses its polarityduring the maximum phase of each activity cycle. Asobserved on the photosphere, active region (AR) magneticflux migrates poleward in narrow, sheared streams resultedfrom large-scale flows and diffusion. A small net flux of thetrailing sunspot polarity eventually aggregates at highlatitudes, manifesting the poloidal field of the next cycle.We characterize this process for the ongoing cycle 24based on four years' line-of-sight magnetograms from theHelioseismic and Magnetic Imager (HMI). The axial dipolecomponent reversed sign in early 2012, but the polewardflux migration was grossly out of phase in the twohemispheres. As a proxy, the northern polar field (taken as

mean above 70 degrees latitude) switched from negative topositive in late 2012, whereas the southern remainedpositive as of March 2014. Three factors that are in linewith the surface flux transport model may havecontributed. First, AR emergence started and peaked earlierin the north. Second, several ARs with small or inverse tiltangles (w.r.t. the Joy's law) emerged in the south in late2010. Third, meridional flow speed inferred fromhelioseismology varied greatly prior to 2013; slowerstreams (compared to a three-year mean at the samelatitude) appeared earlier in the north. We correlate HMIwith the long-running Wilcox Solar Observatory (WSO)dataset, and compare the current cycle with the previousthree.Author(s): Xudong Sun (Stanford University), Jon Hoeksema(Stanford University), Yang Liu (Stanford University), Junwei Zhao (StanfordUniversity)

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104 – Solar Energetic Events IMeeting-in-a-Meeting – Staffordshire – 02 Jun 2014 10:00 AM to 11:30 AMChair(s):Gianna Cauzzi (INAF)

104.01 – Empirical Study of TurbulentDiffusion in Flare Plasma SheetsVelocity fields in the hot (>10 MK) plasma sheets abovepost-eruption flare arcades have the hallmarks of turbulentflow. Tracking and measuring these velocity fields enablesempirical estimation of transport parameters, e.g. turbulentdiffusivity, that are important for determining the spectrumof length scales present in the plasma sheet. Thesetransport parameters thus help to set the rate of magneticreconnection, and may help us to understand howreconnection can be triggered, accelerated, and prolongedin eruptive flares. In this work we show measurements, forthe first time, of transport parameters in flare plasmasheets, enabled by high-resolution observations from SDOand local correlation tracking.Author(s): David McKenzie (Montana State Univ.), Michael Freed(Montana State Univ.)

104.02 – Acceleration of SEPs in FlaringLoops and CME Driven shocksWe consider two stage acceleration of the Solar EnergeticParticles (SEPs). The first occurring via the stochasticacceleration mechanism at the flare site in the corona,which produces the so-called impulsive SEPs, withanomalous abundances, as well as nonthermal particlesresponsible for the observed radiation. The second isre-acceleration the flare accelerated particles at the CMEdriven shock associated with larger, longer duration eventswith relatively normal abundances. Turbulence plays amajor role in both stages. We will show how stochasticacceleration can explain some of the salient features of theimpulsive SEP observations; such as extreme enrichment of3He (and heavy ions), and the observed broad distributionsand ranges of the 3He and 4He fluences. We will then showthat the above hybrid mechanism of first stochasticacceleration of ions in the reconnecting coronal magneticstructures and then their re-acceleration in the CME shockcan produce the varied shapes of the 3He and 4He spectraobserved in all events ranging from weak impulsive tostrong gradual events.Author(s): Vahe Petrosian (Stanford University), Qingrong Chen(Stanford University)

104.03 – Unusual Sunquake EventsChallenge the Standard Model of SolarFlares"Sunquakes" represent helioseismic waves excited by solarflares. According to the standard flare model, sunquakesare associated with the hydrodynamic response of the lowatmosphere to beams of flare-accelerated particles.Observations with the HMI instrument on Solar DynamicsObservatory have shown that sunquakes are a much morecommon phenomenon than this was found from theprevious SOHO/MDI observations. The HMI observationsreveal that sunquakes may occur not only during strongX-class flare but also in relatively weak flares of low M-class(as low as M1). It is particularly surprising that, in somecases, the sunquake initiating impacts are observed in theearly impulsive or even pre-heating phase, prior to themain hard X-ray impulse and even without a significanthard X-ray signal. We examine properties of such sunquakeevents, present a detailed analysis of M2.8 flare of February17, 2013, using HMI, AIA, GOES and RHESSI data, anddiscuss implications for the standard flare model.Author(s): Alexander Kosovichev (Crimean Astrophys.Observatory), Ivan Sharykin (Space Research Institute of RAS), IvanZimovets (Space Research Institute of RAS)

104.04 – Bulk Acceleration of Electrons inSolar Flares?In two recent papers it has been argued that RHESSIobservations of two coronal “above-the-loop-top” hardX-ray sources, together with EUV observations, show thatALL the electrons in the source volumes must have beenaccelerated. I will briefly review these papers and show thatthe interpretation most consistent with the combined flareobservations is multi-thermal, with hot, thermal plasma inthe “above-the-loop-top” sources and only a fraction, albeita substantial fraction, of the electrons accelerated. Thus,there is no credible scientific evidence for bulk accelerationof electrons in flares. Differential emission measure (DEM)models deduced from SDO/AIA and RHESSI data, includingthe inversion of the AIA data to determine DEM, will bediscussed as part of this analysis.Author(s): Gordon Holman (NASA Goddard Space Flight Center)

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104.05 – Inferred Particle Acceleration byContracting Magnetic Islands in MHDSimulations of Flare ReconnectionThe mechanisms that accelerate ionized particles to theenergies required to produce the observed high-energyemission in solar flares are not well understood. Drake et al.(2006) proposed a kinetic mechanism for acceleratingelectrons in contracting magnetic islands formed byreconnection. In this model, particles that gyrate aroundmagnetic field lines transit from island to island, increasingtheir energy by Fermi acceleration in those islands that arecontracting. Macroscopic regions filled with a large numberof these small islands are required to achieve the largeobserved rates of energetic electron production in flares,but at the moment it is impossible to simulate sufficientlylarge-scale systems using kinetic models. Our recenthigh-resolution, compressible MHD simulations of abreakout eruptive flare (Karpen et al. 2012) allow us toresolve in detail the generation and evolution ofmacroscopic magnetic islands in the flare current sheet,and to study the Drake et al. mechanism in a configurationthat more closely represents the flare atmosphere andstructure. Based on the Drake et al. studies, wecharacterize island contractions in our simulations as theislands move away from the main reconnection site towardthe flare arcade. To that end, with our null-trackingcapabilities, we follow the creation and evolution of X- andO-type (island) nulls that result from spatially andtemporally localized reconnection. Preliminary results showthat the initial energy of particles could be increased by upto an order of magnitude in a typical contracting island,before it reconnects with the underlying arcade. Weconclude that this mechanism is a promising candidate for

electron acceleration in flares, but further research isneeded, including extending our results to 3D flareconditions.Author(s): Silvina Guidoni (NASA Goddard Space Flight Center),Judith Karpen (NASA Goddard Space Flight Center), C. DeVore (NASAGoddard Space Flight Center)

104.06 – RHESSI and EIS observations of anabove-the-looptop reconnection regionA variety of solar flare observations suggest particleacceleration in the corona, at or above the flare looptop.Hard X-ray (HXR) studies, for example, occasionally revealaccelerated electrons above flare looptops, in some casessuggesting the location of the acceleration region.However, since coronal HXR sources are faint and thestructure of the flare as seen in extreme ultraviolet (EUV)images is complicated, it is difficult to say where thesesources lie with respect to, for example, the reconnectionregion. HXR and EUV observations can providecomplementary information for investigating this topic. EUVimaging spectroscopy reveals bulk flows and locations ofline-broadened (potentially turbulent) sources. Suchobservations can, for example, identify outflows from thereconnection region. HXR imaging places the flare-accelerated electrons in the context of the overall flaregeometry, allowing comparison of the locations ofaccelerated electrons, the reconnection region, and theflare loop. In this work, data from RHESSI and Hinode/EISare used to investigate above-the-looptop sources in the2013 May 15 X-class flare. Above-the-looptop EIS flows andloop-top line-broadening are compared with RHESSI HXRsources in the preimpulsive phase of the flare.Author(s): Lindsay Glesener (University of California, Berkeley),Hirohisa Hara (National Astronomical Observatory of Japan), Sam Krucker(University of Applied Sciences Northwestern Switzerland)

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105 – Topics in AstrostatisticsSpecial Session – St. George AB – 02 Jun 2014 10:00 AM to 11:30 AM

Modern AstroStatistics has emerged as a new field in recent times, informed by a Bayesian foundation, utilizingpowerful computational tools like MCMC, and applied to diverse analysis and inference problems in Astronomy.The use of statistics to validate results and evaluate models is pervasive in modern astronomy and advancedstatistical techniques have been extensively applied across cosmology, high-energy astrophysics, solar physics,large surveys, etc. Poisson techniques have proliferated, and the use of MCMC is common today. The diversity ofastronomical data has also had positive feedback on Statistics, and has influenced the development of newalgorithms and insights. Now, new methods of data collection, and the rapidly increasing amounts of data that arecollected (the “Big Data” problem), pose new challenges of analysis and interpretation. The goal of our SpecialSession is to review current practices, highlight modern techniques, and explore how the transition into the realmof Big Data Astronomy can be facilitated. Analysis and interpretation of the terabyte and petabyte data streamsfrom forthcoming surveys and missions is a major challenge to the practice of Astronomy, and possibly requires asignificant restructuring of the types of problems that are addressed. A secondary purpose of this Session is tobuild broad community awareness about the risks and rewards of principled analysis. We will explore the pitfallsof using advanced and powerful techniques as black boxes, and will highlight the complexities that arise fromimplementations and broad usage among Astronomers. The session will be complemented by an informalinteractive discussion session hosted at the Chandra Booth as part of a program initiated by theSAO/Harvard-based CHASC AstroStatistics Collaboration. CHASC will arrange for Statisticians to be available atspecified times to answer questions and discuss AstroStatistical issues with Astronomers.

Chair(s):Aneta Siemiginowska (Harvard-Smithsonian, CfA)

Organizer(s):Vinay Kashyap (Harvard Smithsonian, CfA)

105.01 – Towards Good Statistical Practicesin Astronomical StudiesAstronomers do not receive strong training in statisticalmethodology and are therefore sometimes prone to analyzedata in ways that are discouraged by modern statisticians.A number of such cases are reviewed involving theKolmogorov-Smirnov test, histograms and other binnedstatistics, various issues with regression, model selectionwith the likelihood ratio test, over-reliance on `3-sigma'criteria, under-use of multivariate clustering algorithms,and other issues.Author(s): Eric Feigelson (Penn State Univ.)

105.02 – Big Computing in Astronomy:Perspectives and ChallengesHardware progress in recent years has led to astronomicalinstruments gathering large volumes of data. In radioastronomy for instance, the current generation of antennaarrays produces data at Tbits per second, and forthcominginstruments will expand these rates much further. Asinstruments are increasingly becoming software-based,astronomers will get more exposed to computer science.This talk therefore outlines key challenges that arise at theintersection of computer science and astronomy andpresents perspectives on how both communities cancollaborate to overcome these challenges. Major problemsare emerging due to increases in data rates that are muchlarger than in storage and transmission capacity, as well ashumans being cognitively overwhelmed when attemptingto opportunistically scan through Big Data. As aconsequence, the generation of scientific insight willbecome more dependent on automation and algorithmicinstrument control. Intelligent data reduction will have tobe considered across the entire acquisition pipeline. In thiscontext, the presentation will outline the enabling role ofmachine learning and parallel computing. Bio VictorPankratius is a computer scientist who joined MIT HaystackObservatory following his passion for astronomy. He iscurrently leading efforts to advance astronomy throughcutting-edge computer science and parallel computing.Victor is also involved in projects such as ALMA Phasing toenhance the ALMA Observatory with Very-Long BaselineInterferometry capabilities, the Event Horizon Telescope, aswell as in the Radio Array of Portable InterferometricDetectors (RAPID) to create an analysis environment usingparallel computing in the cloud. He has an extensive trackrecord of research in parallel multicore systems andsoftware engineering, with contributions to auto-tuning,debugging, and empirical experiments studyingprogrammers. Victor has worked with major industrypartners such as Intel, Sun Labs, and Oracle. He holds adistinguished doctorate and a Habilitation degree inComputer Science from the University of Karlsruhe. Contacthim at [email protected], victorpankratius.com, or Twitter@vpankratius.

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Author(s): Victor Pankratius (MIT) 105.03 – The Full Monte Carlo: A LivePerformance with StarsMarkov chain Monte Carlo (MCMC) is being appliedincreasingly often in modern Astrostatistics. It is indeedincredibly powerful, but also very dangerous. It is popularbecause of its apparent generality (from simple to highlycomplex problems) and simplicity (the availability of out-of-the-box recipes). It is dangerous because it alwaysproduces something but there is no surefire way to verify oreven diagnosis that the “something” is remotely close towhat the MCMC theory predicts or one hopes. Using verysimple models (e.g., conditionally Gaussian), this talk startswith a tutorial of the two most popular MCMC algorithms,namely, the Gibbs Sampler and the Metropolis-HastingAlgorithm, and illustrates their good, bad, and uglyimplementations via live demonstration. The talk ends witha story of how a recent advance, the Ancillary-SufficientInterweaving Strategy (ASIS) (Yu and Meng, 2011,http://www.stat.harvard.edu/Faculty_Content/meng/jcgs.2011-article.pdf) reduces the danger. It wasdiscovered almost by accident during a Ph.D. student’s(Yaming Yu) struggle with fitting a Cox process model fordetecting changes in source intensity of photon countsobserved by the Chandra X-ray telescope from a(candidate) neutron/quark star.Author(s): Xiao-Li Meng (Harvard University)

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106 – Bridging Laboratory & Astrophysics: AtomsMeeting-in-a-Meeting – St. George CD – 02 Jun 2014 10:00 AM to 11:30 AM

Laboratory astrophysics is the Rosetta Stone that enables astronomers to understand and interpret the cosmos.This session will focus on the interplay between astrophysics with theoretical and experimental studies into theunderlying atomic processes, which drive our Universe.

Chair(s):John Harry Black (Chalmers University of Technology)Organizer(s):Farid Salama (NASA Ames Research Center)

106.01 – Atomic Data Needs forUnderstanding X-ray Astrophysical PlasmasHigh-resolution X-ray data from current satellites exposethe need for high-quality atomic data of all stripes:wavelengths, collisional/radiative rates, and absorptioncross sections. Astro-H, to be launched in 2015, willincrease the available effective area for high-resolution atsome energies by orders of magnitude, bringing the issueinto sharp relief. There have been a number of recentsuccesses of both theoretical calculations and laboratorymeasurements, as well as many remaining atomic dataneeds which hinder scientific progress (e.g Fe XVII lineratios). These include, amongst other issues, accuratewavelength measurements in the soft X-ray band,well-calibrated diagnostic ratios of select lines, andhigh-resolution absorption cross sections for abundant ions.Finally, astrophysical charge exchange, a newly identifiedcontribution to soft X-ray emission, will be discussed. Thisemission arises due to the interaction of highly chargedions with neutral atoms, forming a diffuse background dueto solar wind ions interacting in the heliosphere andpossibly also arising in more distant environments.Author(s): Randall Smith (Smithsonian Astrophysical Observatory)

Contributing teams: AtomDB Team

106.02 – Laboratory Astrophysics Using theElectron Beam Ion TrapX-ray astronomy has seen profound growth in discoveryspace for over a decade resulting almost entirely from thesuccessful operation of three X-ray observatories: Chandra,XMM-Newton, and Suzaku. The high sensitivity, highresolution instrumentation on these satellites haveprovided the X-ray astrophysicists with relativelystraightforward access to powerful line diagnostics thattightly constrain the physical parameters of celestialsources. For example, accurate measurements of transitionenergies, line shapes, and intensities provide quantitativemeasures of a velocity fields, electron densities andtemperatures. X-ray measurements probe sourcesunattainable by any other wavelength bands, such as theregions of accretion disks near black holes, and the hotintracluster medium in clusters of galaxies. Thus, X-rayastronomy in the age of Chandra, XMM-Newton, andSuzaku provides important pieces of the puzzles necessaryto understand the formation and evolution of galaxies,stars, the phenomena near black holes, and the evolutionof the universe as a whole. Unfortunately, accurateunambiguous interpretation of high quality spectra is oftenlimited by the accuracy and completeness of atomic datarather than the uncertainties related to counting statisticsor instrumentation. Starting over twenty years ago, theelectron beam ion trap facility at Lawrence LivermoreNational Laboratory has been used to benchmark spectralmodels used to interpret celestial data, and to addressspecific problems facing the astrophysics community. Morerecently, the portable FLASH-EBIT, built and maintained atthe Max Planck Institute for Nuclear Physics, Heidelbergand coupled to third and fourth generation light sourceshas opened new measurement regimes relavant to the highenergy astrophysics community. Selected results will bepresented. This work performed under the auspices of theU.S. Department of Energy by Lawrence Livermore NationalLaboratory under Contract DE-AC52-07NA27344 and issupported by NASA grants to LLNL and NASA/GSFC.Author(s): Gregory Brown (LLNL)

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106.03 – Assessing atomic data accuracyalong isoelectronic sequencesThe CHIANTI atomic database provides radiative decayrates and electron excitation rates for modelingcollisionally-excited emission lines from 242 ions. Wepresent a new method for assessing atomic data accuracywhereby level populations for specific atomic levels areplotted along isoelectronic sequences. Results arepresented for the helium through fluorine isoelectronicsequences. Generally a smooth variation of population withatomic number is found and so anomalies, often due toproblems with atomic data, can be identified. Oneexception is for the iron ions, which can show levelpopulations an order of magnitude larger than neighboringions. These can be demonstrated to be due to the muchlarger atomic models that are typically run for iron ions.Author(s): Peter Young (George Mason University), Uri Feldman(Artep Inc.)

106.04 – Comprehensive X-ray AbsorptionModels for Atomic Oxygen and NeonAn analytical formula is developed to represent accuratelythe photoabsorption cross sections of oxygen and neon forall energies of interest for X-ray spectral modelingpurposes. In the vicinity of the K-edge, a Rydberg seriesexpression is used to fit R-matrix results, includingimportant orbital relaxation effects, which accuratelypredict the absorption oscillator strengths below thresholdand merge consistently and continuously to the above-threshold cross section. Further minor adjustments aremade to the threshold energies in order to align the atomicRydberg resonances most reliably after consideration ofboth experimental and observed line positions. At energiesfar below or above the K-edge region, the formulation isbased on both outer-shell and inner-shell directphotoionization, including significant shake-up andshake-off processes that result in photoionization-excitationand double photoionization contributions to the total crosssection. The ultimate purpose for developing a definitivemodel for oxygen absorption is to resolve a discrepancybetween the inferred atomic and molecular oxygenabundances in the interstellar medium (ISM) from XSTARand SPEX spectral models.Author(s): Thomas Gorczyca (Western Michigan University), JavierGarcia (Harvard Smithsonian Center for Astrophysics), Manuel Bautista(Western Michigan University), Claudio Mendoza (Instituto Venezolano deInvestigaciones Cientificas), Efrain Gatuzz (Instituto Venezolano deInvestigaciones Cientificas), Timothy Kallman (NASA Goddard Space FlightCenter)

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107 – Astronomy Research and Development Using PicosatellitesSpecial Session – Gloucester, 2nd Floor – 02 Jun 2014 10:00 AM to 11:30 AM

As CubeSats move from rare to ubiquitous parts of college programs, picosatellites for instrument prototyping andfledgling science goals feeds back into professional and amateur astronomy. We discuss current and in-designuniversity graduate and undergraduate research as well as private/society satellite experiments with a science orinstrumentation goal. Topics include in situ measurements of Sun-Earth interaction, amateur-class space-basedimaging, multiple picosatellite constellations, use of picosatellites for undergraduate research, and use ofpicosatellites for prototyping detector concepts.

Chair(s):Alexander Antunes (Capitol College)

107.01 – Profiling near-Earth debris usingpicosatellitesThe 'TrapSat' team at Capitol College adopts Aerogel to doin-orbit and potentially trans-lunar capture and observationof incident debris. We present early test results for thisdetector to measure the mass and distribution of ambientnear-Earth and interplanetary debris. Expected debrisincludes both man-made orbital debris as well asmicrometeorite particles. The theory is that depth imagesshowing penetration of debris into the Aerogel capturemechanism (used successfully in comet capture missions)are transmitted to track the accumulation rate andestimated size of particles. We include a brief discussion ofhow this method can be used for flights beyond near-Earthand compare expected particle densities to the necessarycapture area and mission flight time. Initial testing usinghigh altitude flights are presented, along with indication ofexpected near-Earth distributions and the confidence levelsin using TrapSat to measure the near-Earth environment.Author(s): Alexander Antunes (Capitol College), Ryan Schrenk(Capitol College), Mikus Bormanis (Capitol College), Angela Walters(Capitol College), Travis White (Capitol College)

107.02 – Conducting Science with aCubeSat: The Colorado Student SpaceWeather Experiment (CSSWE)The Colorado Student Space Weather Experiment is a3-unit (10cm x 10cm x 30cm) CubeSat funded by theNational Science Foundation and constructed at theUniversity of Colorado (CU). The CSSWE scienceinstrument, the Relativistic Electron and Proton Telescopeintegrated little experiment (REPTile), provides directionaldifferential flux measurements of 0.5 to >3.3 MeV electronsand 9 to 40 MeV protons. Though a collaboration of 60+multidisciplinary graduate and undergraduate studentsworking with professors and professional engineers, CSSWEwas designed, built, tested, and delivered in 3 years. OnSeptember 13, 2012, CSSWE was inserted to a 477 x 780km, 65° orbit as a secondary payload on an Atlas V throughthe NASA Educational Launch of Nanosatellites (ELaNa)program. The first successful contact with CSSWE wasmade within a few hours of launch. CSSWE then completeda 20 day system commissioning phase which validated theperformance of the communications, power, and attitudecontrol systems. This was immediately followed by anaccelerated 24 hour REPTile commissioning period in timefor a geomagnetic storm. The high quality, low noisescience data return from REPTile is complementary to theNASA Van Allen Probes mission, which launched two weeksprior to CSSWE. On January 5, 2013, CSSWE completed 90days of on-orbit science operations, achieving the baselinegoal for full mission success and has been operating since.An overview of the CSSWE system, on-orbit performanceand lessons learned will be presented.Author(s): Scott Palo (University of Colorado), Xinlin Li (University ofColorado), David Gerhardt (University of Colorado), Lauren Blum(University of Colorado), Quintin Schiller (University of Colorado), RickKohnert (University of Colorado)

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107.03 – Low Radio Frequency PicosatelliteMissionsThe dramatic advances in cubesat and other picosatellitecapabilities are opening the door for scientifically importantobservations at low radio frequencies. Because simpleantennas are effective at low frequencies, and receivertechnology allows low mass and low power instruments,these observations are an ideal match for very smallspacecraft. A workshop on cubesat missions for lowfrequency radio astronomy was held at the Kiss Institute forSpace Sciences, Caltech, to explore mission conceptsinvolving one up to hundreds of picosatellites. One resultfrom this workshop was that there are opportunities forviable missions throughout this large range. For example,the sky-integrated spectral signature of highly redshiftedneutral hydrogen from the dark ages and cosmic dawnepochs can be measured by a single antenna on a singlespacecraft. There are challenging issues of calibration,foreground removal, and RF interference that need to besolved, but the basic concept is appealingly simple. At theother extreme, imaging of angular structure in thehigh-redshift hydrogen signal will require an interferometerarray with a very large number of antennas. In this case theprimary requirement is a sufficiently low individualspacecraft mass that hundreds can be launched affordably.The technical challenges for large arrays are long-termrelative station keeping and high downlink data rates.Missions using several to a few tens of picosatellites canimage and track bright sources such as solar and planetaryradio bursts, and will provide essential validation of

technologies needed for much larger arrays. This work hasbeen carried out at the Jet Propulsion Laboratory, CaliforniaInstitute of Technology, under contract with the NationalAeronautics and Space Administration.Author(s): Dayton Jones (JPL)

107.06 – The Application of the LogoLanguage for Future AstronomicalPocketQubes and CubeSatsThe PocketQube T-LogoQube was a successful test of aLogo based system for future astronomical CubeSats. Theflight and ground software for T-LogoQube is based on theLogo programing language. This flight software is the firstuse of the Logo language for the control of any satellite.The T-LogoQube team is compised of ~50 people(professional mentors, faculty, and students). TheT-LogoQube uLogo based flight system acheived thefollowing goals: (1) Transmission of fours types of packetdata with the RFM22B transceiver. (2) Ability to controlT-LogoQube with a "one line uLogo program". (3) The uLogoVM includes a unigue time stamp for all data. (4) Pastbeacon packets are telemetered for a history ofT-LogoQube. (5) Realtime flight analysis of theMagnetometer to measure spin rate on orbit (6) Ability toupload new uLogo code to extend the on orbit operation.(7) Single torque coil to point the T-LogoQube spin axis inany direction (8) Detection and ability to correct SEUs Wewill present evolution of Logo for future CubeSats for spacebased astronomy projects.Author(s): J. Jernigan (Little H-Bar Ranch)

108 – Fred Adams: Effects of Clusters on Planetary Systems and PossibleConstraints on the Birth Environment of the Solar SystemPlenary Session – America Ballroom North/Central – 02 Jun 2014 11:40 AM to 12:30 PMChair(s):Edward Churchwell (Univ. of Wisconsin)

108.01 – Effects of Clusters on PlanetarySystems and Possible Constraints on theBirth Environment of the Solar SystemMost stars -- and hence most solar systems -- form withingroups and clusters. The first objective of this talk is toexplore how these star forming environments affect solarsystems forming within them via three channels: dynamicalinteractions, elevated radiation fields, and increasedparticle fluxes. The discussion starts with the dynamicalevolution of young clusters; we use N-body simulations tostudy how evolution depends on system size and initialconditions. Multiple realizations of equivalent cases areused to build up a statistical description of these systems,e.g., distributions of closest approaches and radiallocations. These results provide a framework from which toassess the effects of clusters on solar system formation.

Distributions of radial positions are used in conjunction withUV luminosity distributions to estimate the radiationexposure of circumstellar disks. Photoevaporation modelsdetermine the efficacy of radiation in removing disk gasand compromising planet formation. The distributions ofclosest approaches are used in conjunction with scatteringcross sections to determine probabilities for solar systemdisruption. Finally, we determine the distributions ofradioactive nuclei that are provided to circumstellar disks,where they enhance ionization and heating. This workprovides a quantitative (but statistical) determination of theeffects of clusters on forming solar systems. The secondobjective of this talk is to use these results to placeconstraints on the possible birth environments for our ownsolar system.Author(s): Fred Adams (University of Michigan)

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110 – Long Time Domain AstronomySpecial Session – America Ballroom North/Central – 02 Jun 2014 02:00 PM to 03:30 PM

Long time-domain astronomical data sets are becoming increasingly common, and such data sets have enormouspotential value for exploring phenomena lasting longer than a few decades, a human career or lifetime. In stellarastrophysics, there are clearly a number of potential applications of long time-domain data sets. Long-durationphenomena are already being measured for a number of different objects, like eclipsing binaries and pulsatingvariables. New data sets with all-sky photometry have potential to greatly expand the number of objects andkinds of phenomena potentially observable, leading to both new targets for study and new kinds of variability thatcould change or refine our understanding of stellar evolution. Modern (electronic) astronomical data sets arebeing effectively archived and indexed for better access, and older data sets like catalogs, paper records, andplate archives are being converted to electronic format for effective use in modern analyses. This Special Sessionprovides a forum for the general discussion of long time-domain phenomena with various astronomical datasources. Photometric variability is a common theme for the organizers of this special session, but modernlong-duration data sets are now capable of yielding new astrophysics in a number of fields. Proper motion studies,measurements of astrophysical light echoes, and planetary astronomy are all examples of potential areas open toexploration in the long time domain.

Chair(s):Matthew Templeton (AAVSO)

Organizer(s):Arne Henden (AAVSO)

110.01 – Testing Cataclysmic VariableEvolution Models with Light Curves of>10,000 Magnitudes Over >100 years andFully-Corrected to Johnson B & VA combination of magnitudes from the Harvard andSonneberg plates stacks and the AAVSO data base cancreate very well-sampled light curves with >10,000magnitudes and covering all of 1890-2014 for roughly ahundred cataclysmic variables (CVs; novae, novalikes, anddwarf novae). Care must be taken to get all thesemagnitudes into a modern magnitude system. For thearchival plates, these are all close to the B magnitudesystem so that color terms are small, hence, with the use ofmodern B magnitudes for the comparison stars, thesemagnitudes can all be placed onto the Johnson B system.For the archival visual observations, the originalcomparison sequences can always be found, and themagnitudes for the CV and comparisons must be convertedfrom visual to V, so that the reported magnitudes can befully corrected to Johnson V. The uncertainties from theplates and the visual magnitudes can always be beatendown by daily or yearly averaging to typical real total errorbars of ±0.03 mag, and these are always much smallerthan the sampling error arising from flickering and greatlysmaller than the range of variations. These very-well-sampled >100 year Johnson B & V light curves can be usedto test long term evolution models for CVs. With colleagues,I have made light curves for old novae (GK Per from1890-2014 with 47,000 mags, V603 Aql from 1898-2014using 22,722 mags, Q Cyg from 1876-2014 with 6400mags, T CrB from 1855-2014 using 104,000 mags), Z Camstars (Z Cam from 1923-2014 with 90,000 mags), anddwarf novae (SS Cyg from 1896-2014 with 403,800 mags).The relative accretion rate is given by both the average fluxand by the inverse of the average peak-to-peak time forthe dwarf novae. By this means, I have measured thechanges in the accretion rate for many CVs and how theychange on a yearly basis for a century and longer. Theseobservations are directly compared to various CV evolutionmodels. A complex set of agreements and disagreements isfound.Author(s): Bradley Schaefer (Louisiana State Univ.)

110.02 – Light Echoes from LuminousTransients - Status of the Field and FutureProspectsScattered-light echoes from luminous transients(supernovae, luminous blue variables/supernova impostors)are unique in their ability to preserve an observable recordof the state of a transient in outburst for centuries. Unlikeconventional (i.e. intentional) time-series records, thepresence of interstellar dust on the light echo ellipsoid froma given outburst allows photometric and spectroscopicstudy at any epoch where the scattered-light signal reachesa useful signal-to-noise threshold. Additionally, dust locatedat different positions on an outburst's light-echo ellipsoidwill preserve a record of the hemispheric emission of lightfrom the outburst as seen from each dust location, allowingthe degree of asymmetry of an outburst to be studied. Amore recent application of scattered-light echoes employsthe fact that multiple outbursts of high-amplitude, unstable,luminous variables each produce their own light-echoellipsoids and dust located on such ellipsoids provides anopportunity for multiple outbursts to be studied at thesame (modern) epoch. This talk will provide a briefsummary of the evolution of light echoes from use as a toolto map out the interstellar medium around luminous eventsto their richer and more recent use of investigating theoutbursts themselves. Important findings from observationsof scattered-light echoes regarding SN1987A, Cas A, andeta Car will be highlighted and near-term prospects for newwork and new observational opportunities will bepresented.Author(s): Douglas Welch (McMaster Univ.), Armin Rest (SpaceTelescope Science Institute)

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110.03 – The Importance of Long TimeDomain Observations for UnderstandingPulsation in Cepheids and M SupergiantsContinuous monitoring of both Cepheids and type Csemiregular variables is essential for understanding theirpulsation. Cepheids, for example, can undergo regular,periodic, and irregular changes in pulsation period andamplitude that are attributed to stellar evolution, orbitalmotion about companions, and stochastic processes,respectively. All such information helps to characterizeCepheids in terms of physical attributes. Similar informationis also very useful for pulsating M supergiants, which arestill poorly understood in terms of their pulsation. Specificexamples are provided by BC Cyg and ? Cep, the former aM3 supergiant displaying regular pulsation, the latter a M1supergiant apparently pulsating in fundamental andovertone modes. Both appear to provide long-periodextensions of the Cepheid period-mass and period-agerelations.Author(s): David Turner (Saint Mary's Univ.)

110.04 – Decadal monitoring of variables bythe AAVSO communityThe American Association of Variable Stars has been inexistence for over 100 years. First performing monitoringand follow-up observations for Harvard Collegeastronomers, the organization has expanded into followingthousands of variables with a wide variety ofinstrumentation, as well as participating in the discovery oftransient objects and the data-mining of survey catalogs.Several examples of how long, continuous, homogeneouslight curves can yield astrophysical results not possible withshort lifetime surveys will be given.Author(s): Arne Henden (AAVSO)

110.05 – Will R Coronae Borealis EverReturn to Maximum Light?R Coronae Borealis (R CrB) has been in a deep decline foralmost 7 years. Before that, it spent 6 uninterrupted yearsat maximum light. R CrB is the prototype of its eponymousclass of stars, which are very rare, and have many unusualcharacteristics including extreme hydrogen deficiency, andlarge, sudden declines in brightness of 8 magnitudes ormore. These declines are caused by clouds of carbon dustforming near the atmospheres of the stars, which are laterdissipated by radiation pressure. The RCB stars are trueirregular variables in that the timing of their declinescannot be predicted, but several RCB stars are also knownto begin their declines at a particular phase of theirpulsations. There is a wide range of dust formation activityamong these stars, as well as as a wide variation in thelevel of activity for an individual star over time. Long TimeDomain observations of the RCB stars are necessary tounderstand the frequency of their declines, and to giveclues about how and when the dust forms around theseenigmatic stars.Author(s): Geoffrey Clayton (Louisiana State Univ.)

110.06 – Exploring 100+ Year Variabilitywith DASCH: Statistical Methods and RecentResults.The Digital Access to a Sky Century at Harvard (DASCH)project is currently digitizing the roughly 500,000photographic plates maintained by the Harvard CollegeObservatory. The Harvard plate collection covers each pointof the sky roughly 500 to 3000 times from 1885 to 1992,with limiting magnitudes ranging from B=14-18 mag andphotometric accuracy within ±0.1 mag. Productionscanning (roughly 400 plates/day) is proceeding in Galacticcoordinates from the North Galactic Pole and is currently atroughly 40 degrees galactic latitude. The vastness of thesedata makes DASCH unique in its ability to systematicallystudy variability on decade-long time scales across theentire sky. We are developing new statistical miningtechniques to predictively identify the many classes ofstellar variability and explore their long-term behavior, aswell as discover new unusual cases/classes of variability.Most recently, we are working to implement wavelet-basedalgorithms into our mining routines, better allowing us toanalyze localized non-periodic signals. Here we report onthe progress of our mining and machine learning routines,as well as share several of the exciting new discoveries thatare being made with DASCH. We gratefully acknowledgesupport from NSF grants AST-0407380, AST-0909073 andAST-1313370.Author(s): George Miller (Harvard-Smithsonian Center forAstrophysics), Jonathan Grindlay (Harvard-Smithsonian Center forAstrophysics), Edward Los (Harvard-Smithsonian Center for Astrophysics)

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111 – Solar Energetic Events IIMeeting-in-a-Meeting – America Ballroom South – 02 Jun 2014 02:00 PM to 03:30 PMChair(s):Dana Longcope (Montana State Univ.)

111.01 – Characteristics of Sustained >100MeV ?-ray Emissions Observed by Fermi andtheir Association with Solar Eruptive EventsThe Fermi Large Area Telescope (LAT) has detected >20sustained gamma-ray events >100 MeV lasting up to 20hours. Three of these events have been discussed by theLAT Collaboration in two papers. Similar high-energy eventshave been observed earlier and were given the name LongDuration Gamma Ray Flares (LDGRFs; Ryan, 2000). Wediscuss a comprehensive study of the Fermi eventsbeginning with a list of 98 solar eruptive events (SEEs) from2008 to 2012 May with broad/fast (>800 km/s) or >100 keVhard X-ray emission or SEPs with >10 MeV proton fluxesabove 1 proton flux unit. Our study provides the followingcharacteristics of LAT LDGRFs: of 67 disk SEEs, 41 hadbroad/fast CMEs and 20 had both broad/fast CMEs andimpulsive >100 keV emission; 12 of these 20 weredetected by LAT above 100 MeV; no LAT events weredetected in 21 events with broad/fast CMEs when hardX-ray emission was <100 keV; no LAT events were detectedfrom the 31 CMEs originating from behind the disk. Thissuggests that sustained emission appears to require both abroad-fast CME and a flare with impulsive emission >100keV. From our studies of behind-the-limb SEEs and LATfluxes vs heliolongitude, we conclude that the protonsresponsible for the sustained >100 MeV events interactwithin about 20-30 deg. of the active region, but notnecessarily at the footpoints of the flare loops. We also findin a study of all events: >300 MeV proton interactionsproducing the >100 MeV emission begin from <1 min totens of min from the peak of the HXR emission; durations ofthe sustained emission events last from ~30 min to 20 hrs;spectral indices of >300 MeV protons at the Sun range fromabout -2.5 (2012 May 17 GLE) to steeper than -6 (averageabout -4.8); the proton spectrum can both soften andharden in time; the numbers of >500 MeV solar protonsproducing the sustained emission are typically ten-timeslarger than those in the impulsive flare, but there areexceptions; the numbers of >500 MeV protons producingsustained emission is typically ten-times smaller than thenumbers in SEPs and is well correlated, based on a limitednumber of measurements. This work is funded by theNSF/SHINE and NASA's Fermi/GI programs.Author(s): Gerald Share (University of Maryland), Ronald Murphy(Naval Research Laboratory), Allan Tylka (NASA GSFC), Brian Dennis (NASAGSFC), Richard Schwartz (NASA GSFC), Anne Tolbert (NASA GSFC),Stephen White (Air Force Research Laboratory)

111.02 – Modeling Observable Effects OfCanopy Structure On Conduction-drivenEvaporation From Impulsive Energy ReleaseIt is well established that the solar corona displays a highlystructured appearance. The magnetic field is partiallyresponsible for this structuring (e.g. coronal loops), but thecomplex density and temperature distribution of plasmaalong the field also determines appearance. Thisdistribution of plasma may be dictated in part by thecoronal heating mechanism, which might be constant(steady-heating) or impulsive (nanoflares). In the impulsivepicture, reconnection and loop contraction results inmagnetosonic shocks which compress and heat the coronalplasma. Thermal conduction then transports and depositsheat into the chromosphere, resulting in an overpressurethat drives plasma up into the loop (a process referred to aschromospheric evaporation). It is expected, however, thatthe evaporation process will be sensitive to variations ofthe cross-sectional area of the flux tube, due to thestructure of the magnetic canopy above the footpoint. Thepresence of a magnetic canopy may therefore have asubstantial effect on the supply of mass to the corona inresponse to impulsive heating. In this work, we simulatechromospheric evaporation using a 1-D hydrodynamic codethat models a flare loop as a piston shocktube, neglectinggravity and loop curvature. We include a simplified modelof the chromosphere and transition region, and use anozzle-like area profile as a proxy for the canopy variationof the flux tube. We use this code to explore observableeffects of the canopy on evaporative flow velocities, loopemission measure, and coronal mass supply duringimpulsive evaporation.Author(s): Sean Brannon (Montana State Univ.), Dana Longcope(Montana State Univ.)

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111.03 – On the Nature of the EUV LatePhase of Solar FlaresThe EUV late phase of solar flares is a second peak of thewarm coronal emissions (e.g., Fe XVI) many minutes to afew hours after the GOES soft X-ray peak, which was firstobserved by the EUV Variability Experiment (EVE) on boardthe Solar Dynamics Observatory (SDO). The late phaseemission originates from a second set of longer loops (latephase loops) that are higher than the main flaring loops. Itis explained as being caused by either additional heating orlong-lasting cooling. In this paper, we study the role oflong-lasting cooling and additional heating in producing theEUV late phase using the "enthalpy-based thermalevolution of loops'" (EBTEL) experiments. We find that thelong cooling process in late phase loops, which definitelyexists, can sufficiently explain the emission property of theEUV late phase; meanwhile, we cannot exclude the role ofan additional heating of these loops that possibly occurs.Moreover, we provide two preliminary methods based onthe UV and EUV emissions from the Atmospheric ImagingAssembly (AIA) on board SDO to determine whether anadditional heating plays some role or not in the late phaseemission. Through the nonlinear force-free field modeling,we study the magnetic configuration related to the EUV latephase. It is found that the late phase can be generatedeither in hot spine field lines associated with a magneticnull point or large-scale magnetic loops in multipolarmagnetic fields. In this paper, we also explain why the EUVlate phase appears most obviously in the warm coronalemissions and why the majority of flares do not exhibit anEUV late phase.Author(s): Ying Li (Nanjing University), Mingde Ding (NanjingUniversity), Yang Guo (Nanjing University), Yu Dai (Nanjing University)

111.04 – Investigating An X-ClassLong-Duration Confined FlareWe report the observation of an X-class long-duration flarewhich is clearly confined. It appears as a compact-loop(~50 Mm high in projection) flare in the traditional EUVpassbands (171 and 195A}; ~1 MK), but in the passbandssensitive to flare plasmas (94 and 131A; 6-10 MK), itexhibits a cusp-shaped structure above an arcade of loops(~100 Mm high in projection) like other long-durationevents. Inspecting images in a running difference approach,we find that the seemingly diffuse, quasi-staticcusp-shaped structure actually consists of multiple nestedloops that repeatedly rise upward and disappearapproaching the cusp point. Over the gradual phase of theflare, we detect numerous episodes of loop rising, eachlasting minutes. A differential emission measure analysisreveals that the temperature is highest at the top of thearcade and becomes cooler at higher altitudes within thecusp-shaped structure. These features are contrary totypical long-duration flares that conform to the standardflare model. With a nonlinear force-free reconstruction ofthe active region, our analysis of the photosphericsquashing factor $Q$ shows that the configuration haslocally a tri-polar structure, in the middle of which thenegative polarity is divided in half by a high-$Q$ line. Therespective halves belong to two adjacent sheared arcades,one of which harbors a magnetic flux rope. The indicatedhigh-Q line is a footprint of a hyperbolic flux tube (HFT)where two quasi-separatrix layers (QSLs) adjoin each otherat a T-type junction passing through the joint arcades' apex.Comparing UV 1600A flare ribbons with the photosphericQ-maps at close times, we conclude that the emergence ofa new magnetic flux within the arcade void of flux ropetriggers the flare, while the preexisting T-type HFT and fluxrope dictate the structure and dynamics of the observedflare loops and ribbons. The flux rope fails to escape owingto a strong confining field but contributes to thelong-lasting gradual phase with the dissipation of QSLcurrents.Author(s): Rui Liu (University of Science & Technology of China),Viacheslav Titov (Predictive Science Inc.), Tingyu Gou (University ofScience & Technology of China), Yuming Wang (University of Science &Technology of China), Kai Liu (University of Science & Technology ofChina), Haimin Wang (New Jersey Institiute of Technology)

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111.05 – Non-thermal Motions in and AboveFlare Loop Tops Measured by the Extreme-ultraviolet Imaging Spectrometer (EIS) onHinodeThe plasma volume above the soft X-ray emitting loop topsis of particular interest for studying the formation of flareloops. We present EIS observations of non-thermal motions(turbulence) determined from spectral line profiles of FeXXIII and Fe XXIV ions for three well-observed flares nearthe solar limb. We compare the non-thermal motions attemperatures near 10 MK with the motions along the samelines-of-sight determined from lines of coronal ions such asFe XII, Fe XIV, and Fe XV formed at 1-2 MK. The take-awayis that the non-thermal motions obtained from Fe XXIII andFe XXIV lines increase with height towards the reconnectionregion, up to speeds of about 50-60 km/s for the largestheights that we can observe. The implication is thatconsiderable plasma heating occurs outside thereconnection region. In addition, we discuss theimplications of results obtained for flares from earlier X-rayYohkoh observations of line profiles of Fe XXV and Ca XIX onthe current results from EIS and AIA. Fe XXV is formed atsignificantly higher temperatures than any strong flare EUVspectral line observed by EIS or by imaging telescopes suchas AIA or TRACE. This work is supported by NASA grants.Author(s): George Doschek (NRL), David McKenzie (Montana StateUniversity), Harry Warren (NRL)

111.06 – Observations and Implications ofLarge-Amplitude Longitudinal Oscillationsin a Solar FilamentOn 20 August 2010 an energetic disturbance triggeredlarge-amplitude longitudinal oscillations in a large fractionof a nearby filament. The triggering mechanism appears tobe episodic jets connecting the energetic event with thefilament threads. We analyzed this periodic motion tocharacterize the underlying physics of the oscillation aswell as the filament properties. The results support ourprevious theoretical conclusions that the restoring force oflarge-amplitude longitudinal oscillations is solar gravity,and the damping mechanism is the ongoing accumulationof mass onto the oscillating threads. Based on our previouswork, we used the fitted parameters to determine themagnitude and radius of curvature of the dipped magneticfield along the filament, as well as the mass accretion rateonto the filament threads. These derived properties arenearly uniform along the filament, indicating a remarkabledegree of homogeneity throughout the filament channel.Moreover, the estimated mass accretion rate implies thatthe footpoint heating responsible for the thread formation,according to the thermal nonequilibrium model, agrees withprevious coronal heating estimates. We also estimated themagnitude of the energy released in the nearby event bystudying the dynamic response of the filament threads, andconcluded that the initiating event is likely to be amicroflare. We will present the results of this investigationand discuss their implications for filament structure andheating. This work was supported by NASA’s H-SR program.Author(s): Judith Karpen (NASA Goddard Space Flight Center),Manuel Luna (Instituto de Astrofisica de Canarias), Kalman Knizhnik (NASAGoddard Space Flight Center), Karin Muglach (NASA Goddard Space FlightCenter), Holly Gilbert (NASA Goddard Space Flight Center), Therese Kucera(NASA Goddard Space Flight Center), Vadim Uritsky (NASA Goddard SpaceFlight Center)

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112 – Solar Magnetism IIMeeting-in-a-Meeting – Staffordshire – 02 Jun 2014 02:00 PM to 03:30 PMChair(s):Maria Kazachenko (UC Berkeley)

112.01 – New Vector Spectropolarimetry ofSunspots near 4000nmMagnetic sensitivity of spectral lines increases as theproduct of the wavelength and the Lande g-factor. Whilethe most magnetically sensitive spectral line known is theMg I 12318nm line, and observations are often made near1600nm, little work has been done using solar spectrallines near 4000nm We report on new solarspectropolarimetric observations at these wavelengths,made at the NSO McMath-Pierce facility with the NAC andat the NJIT New Solar Telescope using CYRA. Severalphotospheric absorption lines have been used to map asunspot magnetic field, and molecular line Zeeman splittinghas also been observed. Several "negative-g" molecularlines are seen, and an atomic line shows unusual profiles.Author(s): Matthew Penn (National Solar Obs.), Roy Coulter (NewJersey Institute of Technology), Philip Goode (New Jersey Institute ofTechnology)

112.02 – A Spectro-polarimetric Analysis ofSunspot UmbraeThe recent quiet solar cycle has invited new questions as tothe nature of the solar magnetic field and how it changesover time. To investigate this, we use the National SolarObservatory’s McMath-Pierce Solar Telescope Facility(McMP) and Dunn Solar Telescope (DST) to comparemeasurements of sunspots from five active regionsobserved in 2013. Both BABO at the McMP and FIRS at theDST were used to provide spectra of the Fe 1564.8nm line,which is affected by the presence of magnetic fields. Themagnetic field is derived from Zeeman splitting in Stokes-Iby BABO, and by inversion of the Stokes parameters fromFIRS data allowing for comparisons of sunspot propertiesbetween the two instruments.. We present the first resultsfrom this study including the magnetic fields in sunspotumbrae from five active regions measured simultaneouslyby BABO and FIRS.Author(s): Fraser Watson (National Solar Observatory), AlexandraTritschler (National Solar Observatory), Matthew Penn (National SolarObservatory), Christian Beck (National Solar Observatory), WilliamLivingston (National Solar Observatory), Valentin Martinez Pillet (NationalSolar Observatory)

112.03 – Sunspotter: Using Citizen Scienceto Determine the Complexity of SunspotsIt is well known that sunspot groups with large, complexmagnetic field configurations and strong, sheared polarityseparation lines produce the largest flares. While methodsfor determining certain physical properties, such as totalmagnetic flux and polarity-separation-line length have beensuccessfully developed for characterizing sunspot groups, areliable automated method for determining sunspotcomplexity has never been developed. Since complexitycan only be measured in a relative sense, we have usedcrowd-sourcing methods to allow human observers tocompare the complexity of pairs of sunspot groups. Thisallows a large dataset to be ranked in terms of complexity.Sunspotter.org uses the Zooniverse platform and allows thegeneral public to contribute comparisons using aweb-browser interface. The results of this project will helpto establish the true relationship between sunspot groupcomplexity and flares, which has been discussed in thesolar physics community for many decades.Author(s): Paul Higgins (Lockheed Martin), David Perez-Suarez (FMI),Michael Parrish (Adler Planetarium), David O'Callaghan (Trinity CollegeDublin), K Leka (NWRA), Graham Barnes (NWRA), Joseph Roche (TrinityCollege Dublin), Peter Gallagher (Trinity College Dublin)

Contributing teams: Sunspotter Science Team,Zooniverse Development Team

112.04 – AN ANALYTICAL APPROACH TOSCATTERING REGIMES BETWEEN THINMAGNETIC FLUX TUBES WITHIN ANENSEMBLEMotivated by the inability to directly observe the smallscale structure of solar magnetic features. We present ananalytical method to model the multiple scattering regimewithin ensembles of random thin magnetic flux tubes,embedded in a stratified medium. Results demonstrate thatthe near-field interactions play an important role in theresultant scattered wave field. As such the ensemble nolonger behaves as a bunch of individual tubes, rather as alarger collective. It is also shown that the scatteringbetween azimuth orders (m) is as significant as scatteringbetween p-modes. We present a comparison between thisanalytical model and observations, as well as recentnumerical studies.Author(s): Chris Hanson (Monash University), Paul Cally (MonashUniversity)

112.05 – The Sun's Magnetic Field During aGrand Minimum of ActivityDuring a grand minimum of solar activity, no sunspots areobserved on the photosphere, but what might the Sun'smagnetic field look like? One possibility is that there wouldbe no active regions or larger scale magnetic activity. Wehave extended our photospheric model for small-scalemagnetic flux evolution to cover the full Sun. As an initialstudy, we consider how the surface magnetic field of theSun would look if only smaller-scale magnetic features wereallowed to emerge. We also consider the resultant coronaland inner heliospheric magnetic fields, and discusspotential consequences of such fields for Earth.Author(s): Karen Meyer (University of St Andrews), Duncan Mackay(University of St Andrews)

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112.06 – Magnetic Reconnection Above andBelow the Transition RegionThere is little doubt that the plasma environment in thesolar atmosphere varies greatly from the high beta ~1 eVweakly ionized plasmas of the lower chromosphere, to lowbeta ~100 eV conditions in the quiet Sun corona, to thecollisionless ~10 keV plasmas in active flaring regions. Atthe same time, the theoretical considerations of the theknown complexity of evolving solar magnetic fieldstructures, as well as accumulating observational evidence,suggest that the process of magnetic reconnection isubiquitous throughout the solar atmosphere and likelyoccurs under each of the above plasma conditions. Yet, asingle model of magnetic reconnection that could describeits fundamental properties using a common set ofcharacteristics under such disparate set conditions remainselusive. Here, we explore magnetic reconnection in each ofthese solar parameter regimes by way of numericalsimulations while using a single computational framework.We compare the reconnection dynamics in the threeregimes and, in particular, demonstrate three differentpathways for the magnetic fields to reconnect at rates that

only weakly depend on the micro-physics of magneticdissipation. In the collisionless flare regime, theself-consistent formation of short, low aspect ratio currentsheets allows the plasma to readily flow through thedissipation region leading to fast reconnection. In the quietSun corona, it is the process of secondary island formationthat effectively broadens the reconnection region muchbeyond the laminar resistive current sheet prediction,again, reducing its aspect ratio and accelerating thereconnection process. On the other hand, for a range ofplasma parameters in the weakly ionized chromosphere,self-consistently generated excessive thinning of thecurrent sheet and order-of-magnitude electron densityenhancements in the current sheet can also lead to fastreconnection via rapid recombination. We compare andcontrast the three pathways, as well as discuss theprospects for developing a unified parametrized fast solarreconnection model that could capture all three of theseregimes. This work was supported in part by the NASASR&T and LWS TR&T Programs.Author(s): Vyacheslav Lukin (Naval Research Laboratory)

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113 – Extrasolar Planets: DetectionOral Session – St. George AB – 02 Jun 2014 02:00 PM to 03:30 PMChair(s):David Latham (Harvard-Smithsonian, CfA)

113.01 – How Close are the NearestTransiting Exoplanet Systems? UpdatedPlanet Occurrence Rates from Kepler &Implications for TESSHere we consider the most likely distances and apparentmagnitudes of the nearest transiting exoplanet systems. Inpreparation for the next-generation of exoplanet surveys,we would like to know the properties of these systems inorder to optimize survey strategies and plan follow-upobservations. We begin by populating a catalog of nearbystars with planets using occurrence rates estimated fromKepler. For FGK stars, we rely on previously publishedestimates of the planet occurrence rate. For smaller stars,we determine the planet occurrence rate by using our ownplanet detection pipeline to search for additional planetsaround small Kepler target stars. We empirically measurethe planet detection threshold of our pipeline by injectingand recovering transits. After assigning planets to stars, wequery the resulting planet catalog to determine theproperties of the nearest and brightest transitingexoplanets. We will discuss the implications of thissimulated planet population for exoplanet surveys such asTESS, PLATO, MEarth, CARMENES, CHEOPS, ExoplanetSat,ExTrA, HPF, SPECULOOS, and SPIROU. We also consider theobserving resources that will be required to follow up thesesystems with extremely large ground-based telescopes likethe GMT, TMT, and E-ELT.Author(s): Courtney Dressing (Harvard-Smithsonian Center forAstrophysics), David Charbonneau (Harvard-Smithsonian Center forAstrophysics), Peter Sullivan (Massachusetts Institute of Technology),Joshua Winn (Massachusetts Institute of Technology)

113.02 – The Transiting Exoplanet SurveySatellite MissionThe Transiting Exoplanet Survey Satellite (TESS) willdiscover thousands of exoplanets in orbit around thebrightest stars in the sky. In a two-year survey of the solarneighborhood, TESS will monitor more than 200,000 starsfor temporary drops in brightness caused by planetarytransits. This first-ever spaceborne all-sky transit survey willidentify planets ranging from Earth-sized to gas giants,around a wide range of stellar types and orbital distances.TESS stars will typically be 30-100 times brighter thanthose surveyed by the Kepler satellite; thus, TESS planetswill be far easier to characterize with follow-upobservations. For the first time it will be possible to studythe masses, sizes, densities, orbits, and atmospheres of alarge cohort of small planets, including a sample of rockyworlds in the habitable zones of their host stars. Full frameimages with a cadence of 30 minutes or less will provideprecise photometric information for several million starsduring observation sessions of several weeks. The brighterTESS stars will potentially yield valuable asteroseismicinformation as a result of monitoring at a rapid cadence of1 minute or less. An extended survey by TESS of regionssurrounding the North and South Ecliptic Poles will provideprime exoplanet targets for characterization with the JamesWebb Space Telescope (JWST), as well as other largeground-based and space-based telescopes of the future.TESS will serve as the “People’s Telescope,” with datareleases every 4 months, inviting immediatecommunity-wide efforts to study the new planets. The TESSlegacy will be a catalog of the nearest and brightestmain-sequence stars hosting transiting exoplanets, whichwill endure as the most favorable targets for detailed futureinvestigations. TESS has been selected by NASA for launchin 2017 as an Astrophysics Explorer mission.Author(s): George Ricker (MIT), Roland Vanderspek (MIT), DavidLatham (SAO), Joshua Winn (MIT)

Contributing teams: TESS Science Team

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113.03 – Finding the Nearest ExtrasolarPlanets with the Transiting ExoplanetSurvey SatelliteThe Transiting Exoplanet Survey Satellite (TESS) is underdevelopment for NASA's Explorers Program with a plannedlaunch in 2017. Over a two-year mission, TESS will conductan all-sky survey to find transiting planets around dwarfstars in the solar neighborhood using four wide-angleoptical cameras. TESS will spend between 27 and 350 dayscovering each of several hundred thousand target stars. Inorder to predict its yield, we have developed a detailedsimulation of the TESS mission. We model the selection oftarget stars and adopt a planet population from the Keplerresults. Next, we calculate the photometric signal-to-noiseratio TESS will achieve, accounting for photon shot noise,instrumental artifacts, and the background from zodiacallight and unresolved stars. We will present the yields ofdetected planets from the latest simulations, whichcurrently show that TESS should discover over 200 super-Earths and over 400 sub-Neptunes with host stars brighterthan I=12. We will also estimate the false-positive rate fromblended binary stars. These results will allow thecommunity to prepare for follow-up observations usingphotometric and radial-velocity techniques.Author(s): Peter Sullivan (MIT-Kavli Institute), Joshua Winn (MIT-KavliInstitute), Courtney Dressing (Harvard-Smithsonian Center forAstrophysics), David Charbonneau (Harvard-Smithsonian Center forAstrophysics), Tim Morton (Princeton University), Alan Levine (MIT-KavliInstitute), Roland Vanderspek (MIT-Kavli Institute), George Ricker (MIT-KavliInstitute)

113.04 – Preliminary Planet PopulationStatistics With Kepler Q1-Q16We present preliminary extrasolar planet populationstatistics from analysis of the Kepler Q1-Q16 planetcandidate sample. The analysis takes advantage of therecent work on the Q1-Q16 Kepler planet candidate sample,extensive Monte-Carlo transit signal injection and recoverytests of the Kepler Pipeline, and updates to the stellarparameters provided by the Kepler Stellar Working Group.We also explore the sensitivity of the results to alternativeinputs by considering a machine learning generated planetsample, systematics in the stellar sample properties, orbitaleccentricity, and false positive rates.Author(s): Christopher Burke (SETI Institute / NASA Ames), FergalMullally (SETI Institute / NASA Ames), Jessie Christiansen (NEXSCI /Caltech), Daniel Huber (NASA Ames), Jeffrey Coughlin (SETI Institute /NASA Ames), Susan Thompson (SETI Institute / NASA Ames), Jon Jenkins(NASA Ames), Natalie Batalha (NASA Ames)

113.05 – The Impact of the Kepler PipelineDetection Efficiency on the Derived PlanetPopulation StatisticsAnalyses of the published Kepler planet candidatecatalogues which have attempted to constrain theunderlying planet population have thus far been forced toassume a theoretical detection efficiency. We demonstratethe resulting errors that can arise in the calculated planetstatistics, which are substantially larger than reporteduncertainties on the planet statistics. We also present thelatest results from the ongoing study to empiricallymeasure the detection efficiency of the Kepler pipeline viatransit injection and recovery, across multiple quarters andincluding simulated false positives.Author(s): Jessie Christiansen (NASA Exoplanet Science Institute)

Contributing teams: the Kepler Completeness WorkingGroup

113.06 – Earth-Sized Planets in theHabitable Zones of Cool StarsThe primary goal of the Kepler mission is to determine thefrequency of Earth-sized planets in the habitable zone oftheir parent star. Great strides have been made towardsachieving this goal, including the discoveries of Earth-sizedplanets interior to the habitable zone and several super-Earth-sized planets in the habitable zone. A planet that isboth Earth-sized and has an orbit within the habitable zoneof a main-sequence star, however, has remained elusive.We present updates several promising multi-planet systemsthat have Earth-sized, and possibly sub-Earth-sized,candidates in the habitable zone of cool low-mass stars inthe Kepler field of view. We will present our methods ofcombining ground-based observations with transitmodeling in our quest to confirm these planets and discusstheir potential habitability. More than 70% of the stars inour galaxy are M stars, thus confirming these planets willhave profound implications on the number of potentiallyhabitable worlds beyond our Solar System.Author(s): Elisa Quintana (SETI Institute), Thomas Barclay (SETIInstitute)

113.07 – High Contrast LaboratoryDemonstrations with the VortexCoronagraphThe vortex coronagraph, a phase-based coronagraph thathas a small inner working angle and high throughput hasthe potential to enable observations of exoplanets close tonearby stars. Here we describe recent demonstrationexperiments in the High Contrast Imaging Testbed, thathave yielded monochromatic contrasts better than 10^-9,and contrasts of approximately 10^-8 for light of 10%bandwidth.Author(s): Gene Serabyn (JPL)

Contributing teams: The vortex TDEM team

113.08 – Hidden in Starlight: A Search forWidely Separated Substellar-MassCompanionsRelatively few widely separated substellar-masscompanions of planetary systems are known. Thesecompanions can alter the dynamics of planets throughKozai-mechanism-style secular perturbations, and may be acause of the high mean eccentricity of exoplanets. Theorbital periods of such companions are expected to be ofthe order of tens to thousands of years, making themundetectable by time-domain observations such as transit-and radial velocity searches. We have conducted aSpitzer/Infrared Array Camera (IRAC) 3.6 and 4.5 µmimaging search for widely separated substellar-masscompanions with projected separation between 5 to 40arcsec from their parent star. The 36 stars in my samplerange from 4 to 15 pc from the sun, giving a typicalsensitivity of 10 MJ for objects with an orbital radius in therange of 50 to 300 au. This search required advancedPSF-subtraction techniques in order to minimize the innerworking angle and increase sensitivity. In this talk I presentthe results of this search and discuss the data analysismethods we developed for it.Author(s): Alan Hulsebus (Iowa State University), Massimo Marengo(Iowa State University), Joseph Carson (College of Charleston), KarlStapelfeldt (NASA Goddard Space Flight Center)

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113.09 – Recent Contrast MeasurementsMade Using the PICTURE Visible NullingCoronagraphThe PICTURE-B (Planetary Imaging Concept Testbed Using aRocket Experiment - B) sounding rocket mission will use avisible nulling coronagraph to directly image theexozodiacal dust disk of Epsilon Eridani (K2V, 3.22 pc) inreflected visible light down to an inner radius of 1.5 AU (1.7?/D). This mission will demonstrate a number of keytechnologies for future space-based direct exoplanetimaging missions. These include: wavefront sensing and

control using deformable mirrors in space, a lightweight SiC0.5 meter primary mirror and a milliarcsecond-class finepointing system. The mission is scheduled for launch inOctober, 2014. We present laboratory contrastmeasurements made using the PICTURE-B instrument andmodel predictions of exozodiacal dust detection limitsbased on these measurements.Author(s): Christopher Mendillo (UMASS Lowell), Ewan Douglas(Boston University), Susanna Finn (UMASS Lowell), Brian Hicks (NASAGoddard Space Flight Center), Jason Martel (UMASS Lowell), Timothy Cook(UMASS Lowell), Supriya Chakrabarti (UMASS Lowell)

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114 – Bridging Laboratory & Astrophysics: MoleculesMeeting-in-a-Meeting – St. George CD – 02 Jun 2014 02:00 PM to 03:30 PM

Laboratory astrophysics is the Rosetta Stone that enables astronomers to understand and interpret the cosmos.This session will focus on the interplay between astrophysics with theoretical and experimental studies into theunderlying molecular processes, which drive our Universe.

Chair(s):Steven Federman (Univ. of Toledo)Organizer(s):Farid Salama (NASA Ames Research Center)

114.01 – Diffuse Molecular Cloud Chemistry:Successes and ChallengesDiffuse molecular clouds are transitional objects thought toform the bridge between the diffuse atomic medium anddense molecular clouds. As a result, their study is critical toadvancing our understanding of how molecular clouds formfrom, and disperse back into, the interstellar medium (ISM).Due to their intrinsically low opacities, diffuse molecularclouds were thought to harbor relatively simple physics andchemistry. However, numerous ground- and space-basedobservations obtained over a wide wavelength range haveuncovered an unexpected molecular complexity that ispartially unaccounted for in theories of interstellar cloudsand of star and planet formation. The discrepanciesbetween diffuse cloud model predictions and astronomicalobservations are usually driven by only a few- but major-unknowns: the intrinsic complexity of the observed gasstructure in the ISM, a complexity often only partiallyaccounted for in theories, the uncertainties attached tovarious reaction rates or chemical pathways included incurrent theories, or the limitations attached to availableastronomical instrumentation. I will show how concertedefforts between the astronomical, the theoretical and thelaboratory communities have successfully reconcileddifferences between theoretical predictions andastronomical observations of diffuse molecular clouds and Iwill discuss how such collaborative efforts need to bepursued in order to address some of the challenges posedby recent astronomical observations.Author(s): Paule Sonnentrucker (Space Telescope ScienceInstitute)

114.02 – Selected-Ion Infrared Spectroscopyof Small Organic CationsSmall organic cations of interstellar interest are produced inmolecular beams by a pulsed discharge/supersonic nozzlesource. These ions are mass-selected and studied withinfrared laser photodissociation spectroscopy in a time-of-flight mass spectrometer. Infrared spectra are compared tothe predictions of theory (DFT and/or MP2) to elucidate thestructures of these ions, their isomers and the potentialenergy surfaces connecting these. The carbocation speciesstudied include C2H3+, C3H5+, C3H3+, protonatedbenzene, and protonated naphthalene. Protonatednaphthalene has spectral lines relevant for the three of themain Unassigned Infrared Bands (UIR's) seen in emissionfrom interstellar gas clouds. Oxygen-containing ions includeprotonated formaldehyde, formaldehyde cation andmethanol cation. Each of these small organic ions exhibitsmore than one isomer, allowing investigation of themultiple minima on their potential surfaces.Author(s): Michael Duncan (University of Georgia)

114.03 – Decoding the photochemistry ofsimple astrophysical moleculesAn experimental apparatus with two tunable vacuumultraviolet (VUV) lasers in a windowless pump-probeconfiguration with slice imaging detection has been used tostudy the photochemistry of simple astrophysical moleculessuch as N2, NO, CO, and CO2. The VUV pump laser is set atthe desired photodissociation wavelength and the VUVprobe laser is set detect the atom by setting it to excite aone-photon transition in the VUV region and then using avisible photon to ionize the excited atoms. Thephotodissociation of CO2 in the energy region between

94,000.3 and 98,496.4 cm-1 (11.655-12.212eV) is studiedand we have been able to show that all of the energeticallyaccessible photochemical channels occur. CO2+ h? ?

O(3P”J”) + CO(X1?+) h? ? 5.45 eV ? O(1D) + CO(X1?+) h? ?

7.42 eV ? O(1S) + CO(X1?+) h? ? 9.64 eV ? O(3PJ) + CO(a3?)

h? ? 11.46 eV ? C(3PJ) + O2 (X3?J-) h? ? 11.44 eV This is the

first time that all of these channels in CO2 have beendetermined by the direct detection of the atomicfragments. It shows that even simple molecules made up offirst row atoms that do not contain H atoms can dissociateinto spin forbidden products. We have also been able to usethis apparatus to systematically determine the branching

ratios between the 4S, 2D, and 2P states of N atomsproduced in the photolysis of N2 in the wavelength range

from 100,819.7 to 121,870.1 cm-1(12.500-15.110 eV).These examples show that the photodissociation of themajor molecules that occur in the atmospheres of planets,comets, moons and the interstellar medium can be studiedin the windowless region of the VUV spectrum.Acknowledgements: William M. Jackson and Zhou Lugratefully acknowledge the support of the National ScienceFoundation (NSF) under Grant No. CHE-1301501. Cheuk Y.Ng acknowledges the support by the Chemical Sciences,Geosciences and Biosciences Division, Office of BasicEnergy Sciences, Office of Science, (U.S.) Department ofEnergy (DOE) under Contract No. DE-FG02-02ER15306.Author(s): William Jackson (University of California), Cheuk Ng(University of California), Zhou Lu (University of California), Yih Chang(University of California)

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114.04 – Laboratory Studies OfCircumstellar Carbonaceous GrainFormationThe study of the formation processes of dust is essential tounderstand the budget of extraterrestrial organicmolecules. Although dust with all its components plays animportant role in the evolution of interstellar (IS) chemistryand in the formation of organic molecules, little is known onthe formation processes of carbonaceous dust. We reportthe progress that was recently achieved in this domainusing NASA Ames’ COSmIC facility (Contreras & Salama2013, ApJS, 208, 6). PAHs are important chemical buildingblocks of IS dust. They are detected in IDPs and inmeteoritic samples. Additionally, observational, laboratory,and theoretical studies have shown that PAHs are animportant, ubiquitous component of the ISM. The formationof PAHs from smaller molecules has not been extensivelystudied. Therefore, we have performed laboratoryexperiments to study the dynamic processes of carbongrain formation, starting from the smallest hydrocarbonmolecules into the formation of larger PAH and further intonanograins. Studies of IS dust analogs formed from avariety of PAH and hydrocarbon precursors as well as

species that include the atoms O, N, and S, have recentlybeen performed in our laboratory using the COSmIC facilityto provide conditions that simulate IS and circumstellarenvironments. The species formed in the COSmiC chamberthrough a pulsed discharge nozzle plasma source aredetected and characterized with a cavity ringdownspectrometer coupled to a time-of-flight massspectrometer, thus providing both spectroscopic and ionmass information in-situ. Analysis of solid soot particles wasalso conducted using scanning electron microscopy at theUCSC/NASA Ames’ MACS facility. The SEM analysis of thedeposition of soot from methane and acetylene precursorsseeded in argon plasmas provide examples on the types ofnanoparticles and micrograins that are produced in thesegas mixtures under our experimental conditions. Fromthese measurements, we derive information on the sizeand the structure of IS dust grain particles, the growth andthe destruction processes of IS dust and the resultingbudget of extraterrestrial organic molecules.Acknowledgements: This work is supported by NASA SMD(APRA; Carbon in the Galaxy).Author(s): Cesar Contreras (BAER Institute), Ella Sciamma-O'Brien(BAER Institute), Farid Salama (NASA Ames Research Center)

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115 – Cosmology, CMB, and Dark MatterOral Session – Gloucester, 2nd Floor – 02 Jun 2014 02:00 PM to 03:30 PMChair(s):Melanie Simet (Carnegie Mellon University)

115.01D – Light Curves of Type IaSupernovae and Cosmological Constraintsfrom the ESSENCE SurveyThe ESSENCE survey discovered 213 type Ia supernovae atredshifts 0.10 < z < 0.81 between 2002 and 2008. Wepresent their R and I band light curve measurements,obtained using the MOSAIC II imager at the CTIO 4m, alongwith rapid response spectroscopy for each object from arange of large aperture ground based telescopes. We detailour program to obtain quantitative classifications andprecise redshifts from our spectroscopic follow-up of eachobject. We describe our efforts to improve the precision ofthe calibration of the CTIO 4m natural photometric system.We use several empirical metrics to measure our internalphotometric consistency and our absolute calibration of thesurvey. We assess the effect of various sources ofsystematic error on our measured fluxes, and estimate thatthe total systematic error budget from the photometriccalibration is ~1%. We combine 108 ESSENCE SNIa thatpass stringent quality cuts with a compilation of 441 SNIafrom 3 year results presented by the Supernova LegacySurvey and Baryon Acoustic Oscillation measurements fromthe Sloan Digital Sky Survey to produce cosmologicalconstraints employing the SNIa. This constitutes the largestsample of well-calibrated, spectroscopically confirmed SNIato date. Assuming a flat Universe, we obtain a joint

constraint of ?M = 0.266 +0.026-0.016 (stat 1-?), and w =

-1.112 +0.069 -0.072 (stat 1-?). These measurements areconsistent with a cosmological constant.Author(s): Gautham Narayan (NOAO)

Contributing teams: The ESSENCE Project

115.02 – Galaxy shapes and IntrinsicAlignments in the MassiveBlack-IISImulationThe intrinsic alignment of galaxy shapes with thelarge-scale density field is a contaminant to weak lensingmeasurements, as well as being an interesting signature ofgalaxy formation and evolution (albeit one that is difficultto predict theoretically). Here we investigate the shapesand relative orientations of the stars and dark matter ofhalos and subhalos (central and satellite) extracted fromthe MassiveBlack-II simulation, a state-of-the-art highresolution hydrodynamical cosmological simulation which

includes stellar and AGN feedback in a volume of (100h-

1Mpc)3. We consider redshift evolution from z = 1 to 0.06and mass evolution within the range of subhalo masses,

1010 - 6.0 × 1014.0h-1M?. The shapes of the dark matterdistributions are generally more round than the shapesdefined by stellar matter. We find that the shapes of stellarand dark matter are more round for less massive subhalosand at lower redshifts. By directly measuring the relativeorientation of the stellar matter and dark matter ofsubgroups, we find that, on average, the misalignmentbetween the two components is larger for less massivesubhalos. The mean misalignment angle varies from ?

30°-10° for M ? 1010 - 1014 h-1M? and shows a weakdependence on redshift. We also compare themisalignment angles in central and satellite subhalos atfixed subhalo mass, and find that centrals are moremisaligned than satellites.Author(s): Ananth Tenneti (Carnegie Mellon University), RachelMandelbaum (Carnegie Mellon University), Tiziana DiMatteo (CarnegieMellon University), Yu Feng (Carnegie Mellon University), NishikantaKhandai (Brookhaven National Laboratory)

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115.03 – Observation of DiscreteOscillations in the Plot of CosmologicalScale Factor vs. Lookback TimeWe have observed damped longitudinal cosmological-scaleoscillations in a unique model-independent plot of scalefactor against lookback time. We measured 2 full, constantfrequency, oscillations with a period of 0.15 Hubble times.This period corresponds to a fundamental frequency ofapproximately 7 cycles over the age of the universe, whichwe term 7 “Hubble-Hertz” (HHz). Transition-z values quotedin the literature generally fall near these oscillation minimaand may explain the reported spread and deviation fromthe predicted ?CDM value of approximately z = 0.77. Wealso observe second and third harmonics of thefundamental consistent with the spectrum of a sawtoothwaveform. We propose a cosmological scalar field dampedsimple harmonic oscillator model for the observation –which fits well. On this time scale, the scalar field particlemass is extraordinarily small at 10^ -32 ev. Particles on thisscale have been suggested in the literature as beingassociated with massive gravitons, in which case we maybe observing longitudinal mode gravitational waves. Amultiverse 5-D brane collision scenario is one possiblesource for the scalar field and waves. This scenario enablesan estimate of the compacted 5th dimension radius atapproximately 1,000,000 ly – the size of a galaxy darkmatter halo. Our scalar field density parameter preciselyreplaces the ?CDM dark matter density parameter in theFriedmann equations, resulting in identical data fits, and itspresent value matches the Planck value. We therefore positthat this scalar field manifests itself as the dark matter.Author(s): Harry Ringermacher (Dept. of Physics & Astronomy, U.of Southern Mississippi), Lawrence Mead (Dept. of Physics &Astronomy, U. of Southern Mississippi)

115.04 – A Statistical Test of theRelationship between Galactic HI Structureand Small-scale Structure in the CosmicMicrowave BackgroundThe archive of IRIS, PLANCK and WMAP data available atthe IRSA website of IPAC allows the apparent associationsbetween galactic neutral hydrogen (HI) features andsmall-scale structure in WMAP and PLANCK data to beclosely examined. In addition, HI new observations madewith the Green Bank Telescope are used to perform astatistical test of putative associations. It is concluded thatattention should be paid to the possibility that some of thesmall-scale structure found in WMAP and PLANCK dataharbors the signature of a previously unrecognized sourceof high-frequency continuum emission in the Galaxy.Author(s): Gerrit Verschuur (University of Memphis)

115.05 – Polarization Measurements ofRadio Sources at 43 and 95 GHz in the Q/UImaging Instrument's Cosmic MicrowaveBackground SurveyWe present polarization measurements of extragalacticpoint sources that were observed during the CosmicMicrowave Background polarization survey of the Q/UImaging Experiment (QUIET) at Q-band (43 GHz) andW-band (95 GHz). The sources we examined were selectedfrom the public catalog of the Australia Telescope 20 GHz(AT20G) survey. About 480 sources lie within the fourpatches that QUIET surveyed (totaling ~ 1000 sq. deg.). Wedetect significant linear polarization for several sources ineach frequency band. For the other sources we set limits onthe polarized emission. Finally, we compare our polarizationmeasurements to intensity and polarization measurementsof the same sources from the literature.Author(s): Kevin Huffenberger (Florida State University)

Contributing teams: QUIET collaboration

115.06 – Results from the first season ofPOLARBEAR observationsPOLARBEAR is a Cosmic Microwave Background (CMB)polarization experiment operating in the Atacama Desert inChile since Spring 2012. The instrument covered 30 squaredegrees on the sky, using 1200 bolometric detectorssensitive in polarization with a resolution of 3.5 arcminutes,leading to one of the deepest CMB polarization maps inexistence. The first season of observations withPOLARBEAR was dedicated to searching for CMB B-modepolarization generated by the gravitational lensing inducedby large scale structure. We will describe the experiment,its performance and the latest results derived from its dataset.Author(s): Josquin Errard (Lawrence Berkeley National Lab)

Contributing teams: The POLARBEAR collaboration

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115.07 – Constraints on dark matterannihilation by radio observations of MilkyWayWIMP annihilation in the Milky Way (MW) halo is expectedto produce various energetic stable particles. Theseparticles can manifest themselves through various emissionprocesses. Such an emission spans almost the wholespectrum from radio to gamma bands. In a recent fewyears several groups reported the significant gamma rayexcess at GeV energies in the MW center region, whichcan’t be explained by conventional astrophysical sources.To explain this excess, one needs either an additionalpopulation of millisecond pulsars or the annihilating darkmatter (DM). In the DM scenario, one may estimate thenecessary WIMP properties. And several groups reportrather close WIMP parameters needed: the annihilationcross section around the thermal relic value

<?v>?(1-3)×10-26 cm3/s, low mass m??(10-50) GeV and adominant annihilation into b-anti(b) pairs. Naturally, weexpect a radio counterpart of this gamma excess to bepresent, which originates as a synchrotron radiation ofleptons produced by WIMP annihilation. And acomprehensive study of such a counterpart has not beenconducted yet. Our work is in progress and focused on thelow frequency emission. We are planning to present the

general constraints on WIMP properties based on whole skyradio observations of MW (involving various radio surveysand Planck data), and also planning to support or weakenthe DM interpretation of the gamma excess through studiesof its expected synchrotron counterpart. According to ourpreliminary results, the WIMP parameters mentioned abovemay cause a serious tension with the correspondingobservations, which may, in turn, provide new clues for theDM interpretation of the gamma excess.Author(s): Andrey Egorov (University of Southern California),Jennifer Siegal-Gaskins (California Institute of Technology), Elena Pierpaoli(University of Southern California)

115.08 – An X-Ray Line from eXciting DarkMatterThe recently reported 3.5 keV line from galaxy clusters andM31 has rekindled interest in dark matter production oflines at X-ray energies. We propose a model in which WIMPsare collisionally excited and de-excite via photonproduction, thereby converting WIMP kinetic energy intophotons. Such a mechanism has different dependencies ondensity and velocity than sterile neutrino decay, and hasmore flexibility for explaining the data. I will summarize thecurrent observational status of the 3.5 keV line and themerits of various scenarios to explain it.Author(s): Douglas Finkbeiner (Harvard Univ.), Neal Weiner (NewYork University)

116 – Jacqueline van Gorkom: Gas and Galaxy Evolution: from Voids toClustersPlenary Session – America Ballroom North/Central – 02 Jun 2014 03:40 PM to 04:30 PMChair(s):Paula Szkody (Univ. of Washington)

116.01 – Gas and Galaxy Evolution: fromVoids to ClustersOur understanding of the growth of large scale structurehas advanced enormously over the last decade, thanks toan impressive synergy between theoretical andobservational efforts. The formation and evolution ofgalaxies within these structures is less well understood andespecially the details of the gas physics during accretionand outflow are still controversial. Hydrogen images canhelp distinguish between growth by mergers and accretionof gas, and between inflow and outflow. I will show resultsof HI imaging surveys of galaxies in the local universe in a

wide range of environments, from the deepestunderdensities of voids to the cores of galaxy clustersconfirming some of the general trends seen in simulations.Small galaxies in voids still seem to accrete gas, andgalaxies in clusters are losing it fast. Until recently these HIimaging surveys could not go beyond z~0.1. This haschanged dramatically with the upgrade of the Very LargeArray. I will present the very first results of CHILES, theCOSMOS HI Large Extragalactic Survey, a 1000 hour JVLAsurvey for which the first observations started this fall. Thesurvey will cover one pointing in the COSMOS field, andimage in HI hundreds of galaxies from z=0 to z=0.45.Author(s): Jacqueline Van Gorkom (Columbia Univ.)

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117 – George Ellery Hale Prize, Tom Duvall: Waves Excited by Noise:Applications to Helioseismology and BeyondPlenary Session – America Ballroom North/Central – 02 Jun 2014 04:30 PM to 05:20 PMChair(s):Leon Golub (SAO)

117.01 – Waves Excited by Noise:Applications to Helioseismology and BeyondThe vigorous granular convection just beneath the solarphotosphere excites acoustic waves. The resultant normalmodes of the whole Sun are analogous to the ringing of abell in a sandstorm. In classical helioseismology, the normalmodes are used to study global solar properties, includingthe sound speed versus radius throughout the Sun and therotation rate versus depth and latitude in the outer half ofthe Sun. But solar astronomers wished to better understandthe subphotospheric 3-d structure of smaller scale featuresobserved in the photosphere and were hence not satisfiedstudying only these global properties. One would like tohave something akin to seismology, in which the wavesfrom an earthquake traveling from a source through theinterior to a distant receiver depend only on the propertiesalong the path. However, the random nature of the solarconvective wave sources generally prevents such a simpleanalogy. It was discovered that the temporal cross

correlation of the solar oscillation signal between twolocations averaged over many wave periods does mostlycontain information about the properties along the pathconnecting the two locations. This discovery is the basis fortime-distance helioseismology, in which travel times areextracted from the temporal cross correlations and mappedfor different pairs of locations on the solar surface. Asubsequent 3-d tomography aims to map the solar interior.This technique has been used to study the depth variationof a variety of solar photospheric features from smallspatial scales (granulation) to larger scales (sunspots andsupergranulation) to the largest scales (meridionalcirculation and rotation). The technique of temporal crosscorrelation of noise signals from two locations hassubsequently been adopted successfully in a number ofother fields including seismology, ultrasound, infrasound,ocean acoustics, structural engineering, lunar seismology,and medical diagnostics.Author(s): Thomas Duvall (NASA Goddard Space Flight Center)

118 – Jonathan Grindlay: Time Domain Astronomy with the Harvard Plates:from Cepheids to DASCHPlenary Session – America Ballroom North/Central – 02 Jun 2014 06:30 PM to 07:20 PMChair(s):Chryssa Kouveliotou (NASA/MSFC)

118.01 – Time Domain Astronomy with theHarvard Plates: from Cepheids to DASCHThe ~500,000 Harvard glass plate photographic negativesare the world’s largest and most complete (full sky; 107ytime span) database for Time Domain Astronomy (TDA) ondays-months-decades to century timescales. With plate

fields of view ranging from 3o – 30o exposed quasi-randomly full sky from 1885 – 1992, any object is observed~1000 - 3000 times, with limiting magnitudes ranging fromB =12-18. I briefly review some of the colorful history ofthis massive plate-taking project and a few of the pivotaldiscoveries (e.g. the “Leavitt Law” for the Cepheid Period-Luminosity relation) made by visual studies of the plates bythe true TDA pioneers, the likely <300 different visual usersof the plates. I then describe our Digital Access to a SkyCentury @ Harvard (DASCH) project to fully digitize andreduce this wealth of data (~1 Pb) and provide it onspinning disk to the full astronomical community andpublic. Using the full-sky APASS catalog giving BVR

magnitudes (for V ~9-17) as well as GSC2.3.2 for bothfainter and brighter stars, DASCH does spatially resolved

(0.25o -0.6o bins) photometric calibrations to derive Bmagnitudes with rms~0.1mag over the full plate and overthe (typically) ~6-8 different principal plate series(telescopes and plate scales) covering any given object,along with ~0.3-1 arcsec astrometry (depending on platescale) for each stellar object averaged over ~1year. Thehigh speed/precision scanner, plate processing, andanalysis pipeline have now enabled the first data releases(DR1-DR3) of 12 to cover full sky and already enabled awealth of new discoveries. I describe a few examples, suchas: K2III giants with decadal variations; a new class ofSymbiotic novae; ~50-100y recurrence times for black holeX-ray binary outbursts; and QPOs from 3C273. The DASCHdata are increasingly available (~15% now; 100% in 3.5y)for TDA on largely unexplored timescales. We are gratefulto NSF for support with grants AST-0407380, AST-0909073and AST-1313370.Author(s): Jonathan Grindlay (Harvard-Smithsonian, CfA)

200 – Sara Seager: Mapping the Nearest Stars for Exotic Habitable WorldsPlenary Session – America Ballroom North/Central – 03 Jun 2014 08:30 AM to 09:20 AMChair(s):Steven Federman (Univ. of Toledo)

200.01 – Mapping the Nearest Stars forExotic Habitable WorldsExoplanets are planets orbiting stars other than the sun.Thousands of exoplanets are known and thousands of moreplanet candidates have been found. Until now, thedominant focus on habitable worlds has been on Earth-likeplanets, because Earth is the only known planet with life.Yet exoplanets are astonishingly diverse—in terms of theirmasses, densities, orbits, and host star types—and thisdiversity motivates a radical extension of what

conventionally constitutes a habitable planet. The race tofind habitable exoplanets has accelerated with therealization that “big Earths” transiting small stars can beboth discovered and characterized with current technology.Moreover, technology for space-based direct imaging ofEarth analogs has been rapidly maturing. The ambitiousgoal of inferring signs of life via biosignature gases in anexoplanet atmosphere, once only a futuristic thought, isnow within reach.Author(s): Sara Seager (Massachusetts Institute of Technology)

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– LAD Posters TuesdayPoster Session – Essex Ballroom and America Foyer – 03 Jun 2014 09:00 AM to 06:30 PM

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218.01 – Daily Normalized Helicity ofSubsurface FlowsFlare-productive active regions are associated withsubsurface flows with large values of kinetic helicitydensity. Kinetic helicity is related to mixing and turbulenceof fluids. Reinard et al. 2010 have developed a parameterthat captures the variation of kinetic helicity with depth andtime, the so-called Normalized Helicity Gradient Variance(NHGV). This parameter increases 2-3 days before a flareoccurs and the NHGV values for flaring and non-flaringactive regions represent clearly separate populations. Wederive subsurface flows from the surface to a depth of 16Mm using GONG and SDO/HMI Dopplergrams analyzed withthe ring-diagram technique and calculate kinetic helicitydensity as a function of position on the solar disk. We willthen calculate the NHGV parameter exploring differentnormalization schemes and depth ranges. We will presentcases studies of active regions observed with GONG andSDO/HMI.Author(s): Rudolf Komm (National Solar Observatory), AlyshaReinard (University of Colorado & NOAA/SWPC), Frank Hill (National SolarObservatory)

218.02 – A solar type II radio burst fromCME-coronal ray interaction: simultaneousradio and EUV imagingSimultaneous radio and extreme ultraviolet(EUV)/white-light imaging data are examined for a solartype II radio burst occurring on 2010 March 18 to deduce itssource location. Using a bow-shock model, we reconstructthe 3-dimensional EUV wave front (presumably the type-IIemitting shock) based on the imaging data of the twoSTEREO spacecraft. It is then combined with theNan\c{c}ay radio imaging data to infer the 3-dimensionalposition of the type II source. It is found that the type IIsource coincides with the interface between the CME EUVwave front and a nearby coronal ray structure, providingevidence that the type II emission is physically related tothe CME-ray interaction. This result, consistent with thoseof previous studies, is based on simultaneous radio andEUV imaging data for the first time.Author(s): Yao Chen (Institute of Space Sciences), Guohui Du(Institute of Space Sciences)

218.03 – Validating Time-DistanceHelioseismology With Realistic Quiet SunSimulationsLinear time-distance helioseismic inversions are carried outfor vector flow velocities using travel times measured fromtwo ~100^2 Mm^2 x 20 Mm realisticmagnetohydrodynamic quiet-Sun simulations of about 20hr. The goal is to test current seismic methods on thesestate-of-the-art simulations. We find that horizontal flowmaps correlate well with the simulations in the upper ~3Mm of the domains for several filtering schemes, includingphase-speed, ridge, and combined phase-speed and ridgemeasurements. In several cases, however, the velocityamplitudes from the inversions severely underestimatethose of the simulations, possibly indicating nonlinearity ofthe forward problem. We also find that results of theinversions for the vertical velocity component dependsignificantly on the type of data filtering. In particular,phase-speed filters show better results than the othermethods. In many cases, the vertical flows are irretrievabledue to high levels of noise, suggesting a need for statisticalaveraging.Author(s): Kyle DeGrave (New Mexico State University), JasonJackiewicz (New Mexico State University), Matthias Rempel (HAOUniversity Corporation for Atmospheric Research )

218.04 – The Divergence of CME andSunspot Number Rates During Solar Cycle24In the previous three solar cycles the frequency ofoccurrence of CMEs observed in white light has closelytracked the solar cycle in both phase and amplitude,varying by an order of magnitude over the cycle. LASCOhas now observed the entire solar Cycle 23 and continuesto observe through the current rise and maximum phasesof Cycle 24. Cycle 23 had an unusually long decline andextended minimum. During this period we have been ableto image and count CMEs in the heliosphere, and candetermine rates from both LASCO and STEREO SECCHI(since 2007) coronagraphs and from the Solar MassEjection Imager (SMEI – since 2003) and the SECCHIHeliospheric Imagers in the heliosphere. Manual ratesestimated by observers are now supplemented by countsfrom identifications made by automatic programs, such ascontained in the SEEDS, CACTus and ARTEMIS catalogs.Since the cycle 23/24 minimum, the CME and sunspotnumber rates have diverged, with similar cycle 23/24 riseand peak CME rates but much lower SSN rates in this cycle.We will discuss these rate estimates and their implicationsfor the evolution of the global solar magnetic field.Author(s): David Webb (Boston College), Orville St. Cyr (NASA/GSFC),Hong Xie (NASA/GSFC), Thomas Kuchar (Boston College)

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218.05 – Studying Shallow Meridional Flowby Time-Distance Helioseismology duringthe Rising Phase of Cycle 24Using continuous SDO/HMI Doppler observations, we havestudied the solar subsurface torsional oscillation andmeridional flow during the rising phase of solar cycle 24.The faster bands of the torsional oscillation pattern showclear temporal variations in both width and strength, andthe band in the northern hemisphere extends past theequator into the southern hemisphere. The meridional-flowspeed drops substantially with the rise of magnetic activity,and at some depths and for some brief periods, the floweven reverses directions in mid-latitudes. The residualmeridional flow shows faster and slower bands like thetorsional oscillation patterns, but its faster bands approachthe equator earlier than the torsional oscillation bands.More interestingly, the meridional flow speed in latitudesabove 35 degree slows down (speeds up) when thefollowing-polarity (leading-polarity) magnetic flux istransported poleward, essentially delaying the magneticpolarity reversal and the onset of the next solar cycle.Author(s): Junwei Zhao (Stanford Univ.), Alexander Kosovichev (NewJersey Institute of Technology), Richard Bogart (Stanford Univ.)

218.06 – New Insights into the PhysicalNature of Coronal Mass Ejections within theFramework of the Three-dimensionalStructuresWe present new insights into the physical nature of coronalmass ejections (CMEs) within the framework of the three-dimensional (3D) structures. We have developed a forward-fitting method in order to determine the three-dimensionalstructures of multiple fronts comprising a CME, using datasets taken from STEREO Behind, SOHO and SDO, andSTEREO Ahead. We applied the method to time seriesobservations of a CME on 7 March 2012 and theobservations from the three different perspectives showedthe whole structure of the CME from footprints, so-calledEUV waves, to the top, so-called leading edges, through thelateral flanks. From the analyses, we revealed that a CMEcould consist of two different fronts in the 3D structures:the one is represented well with a shape of ellipsoid,implying that CMEs are bubble-like structure and the otheris reproduced well with a shape of graduated cylindricalshell (GCS), indicating that CMEs are flux rope-likestructure. The bubble structure is seen as the outermostedge of the CME and pass through coronal streamers(global magnetic separatrices). The footprint of the bubbleis the EUV wave front propagating against the solar disk. Inaddition, the bubble is found to be the front comprising ahalo CME in white light observations. On the other hand,the flux rope structure is seen as the three part morphologyhaving fixed legs and cannot pass through coronalstreamers. From our results, we concluded that (1) a CMEcould have both structures, bubble and flux rope-likestructure, (2) the bubble is in fact fast magnetosonicwave/shock front while the flux rope structure is the masscarried outward by underlying magnetic structures, (3) EUVwave is the footprint of the wave bubble, and (4) thecircular front of the halo CME is the wave bubble.Author(s): Ryun Young Kwon (George Mason University), Jie Zhang(George Mason University)

218.07 – Using Synthetic Data FromConvection Simulations To Test HelioseismicHolography Inversions For Three-Dimensional Vector FlowsWe investigate the efficacy of helioseismic holography forinferring the three-dimensional vector flows in thenear-surface layers of the solar interior. Synthetichelioseismic data are taken from compressible convectionsimulations. Travel times are measured from the syntheticdata using helioseismic holography. Kernels for thesensitivity of travel times to subsurface flows are calculatedusing the Born approximation. Inversions for subsurfaceflows are then performed using subtractive optimallylocalized averaging. This provides an opportunity toevaluate the accuracy of the inversion technique. Wecompare the actual flows present in the convectionsimulations to the flows retrieved by the inversion. Wediscuss the influence of the regularization used by theinversion, and the effects of noise and spatial resolution.This work is supported by the NASA SDO Science Centerprogram (NNH09CE41C), the NASA Heliophysics GuestInvestigator program (NNH12CF68C), and the NASA LWSTR&T tools and methods program (NNH09CF68C). TheNational Center for Atmospheric Research is sponsored bythe National Science Foundation.Author(s): Ashley Crouch (NorthWest Research Associates), AaronBirch (Max Planck Institute for Solar System Research), Douglas Braun(NorthWest Research Associates), Brenda Javornik (NorthWest ResearchAssociates), Matthias Rempel (National Center for Atmospheric Research)

218.08 – Developing 3D CME ModelsWe describe the development of CME models in threedimensions, including the energization of active regionsand the initiation of eruptions via flux cancellation. Wecontrast the dynamics from idealized zero-beta models withmore sophisticated models based on thermodynamicsolutions. We explore the effect of the strength of themagnetic field in the active region (or, more appropriately,the amount of smoothing applied to the observed magneticfield), the profiles for transverse field emergence or appliedshear, and the nature of the flux cancellation, on thedynamics of eruptions. In particular, our interest is inunderstanding which effects lead to fast CMEs.Author(s): Zoran Mikic (Predictive Science, Inc.), Tibor Torok(Predictive Science, Inc.), Viacheslav Titov (Predictive Science, Inc.), JonLinker (Predictive Science, Inc.), Kathy Reeves (Harvard Smithsonian)

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218.09 – Observed properties of Giant CellsThe existence of Giant Cells has been suggested by boththeory and observation for over 45 years. We have trackedthe motions of supergranules in SDO/HMI Doppler velocitydata and find larger (Giant Cell) flows that persist formonths. The flows in these cells are clockwise aroundcenters of divergence in the north and counter-clockwise inthe south. Equatorward flows are correlated with progradeflows - giving the transport of angular momentum towardthe equator that is needed to maintain the Sun’s rapidequatorial rotation. The cells are most pronounced at mid-and high-latitudes where they exhibit the rotation ratesrepresentative of those latitudes. These are clearly large,long-lived, cellular features, with the dynamicalcharacteristics expected from the effects of the Sun’srotation, but the shapes of the cells are not wellrepresented in numerical models. While the Giant Cell flowvelocities are small (<10 m/s), their long lifetimes shouldnonetheless substantially impact the transport of magneticflux in the Sun’s near surface layers.Author(s): David Hathaway (NASA/MSFC), Lisa Upton (The Universityof Alabama, Huntsville), Owen Colegrove (University of Rochester)

218.10 – CME Mass Estimates via EVECoronal Dimmings for X-class FlaresThe EVE instrument on SDO detects post-flare dimmings,mainly in the spectral regions of Fe IX-XII in its MEGS-Arange, which is available for most of the 29 X-class flaresthat have occurred between SDO launch and the end ofApril 2014. Based upon earlier X-ray observations weinterpret these dimmings as the result of CME massejection from the low corona. We estimate the massesinvolved in these dimmings by deriving a best pre-eventtemperature and emission measure in the dimmed regionfrom EVE, and a source volume from AIA images. Thedimming for SOL2011-02-15, the first of these events,"peaked"at -3.4% in Fe IX in terms of the pre-eventemission from the whole Sun, with smaller relativedepletions in higher ionization states of Fe. The "maximum"occurred more than one hour after GOES peak. Thedimming signature is generally cleanly measurable in theEVE/MEGS-A spectral samples at 10 s cadence, with thedominant source of uncertainty stemming from the "sun-as-a-star" integrations; for example flare-related excessemission at a given wavelength tends to compensate forthe dimming, and in this sense the mass estimate must beconsidered a lower limit. We address these uncertainties forthe solar case by appealing to the AIA images, but foranalogous processes in stellar flares one would not havethis luxury.Author(s): Hugh Hudson (University of Glasgow), Iain Hannah(University of Glasgow), Karel Schrijver (Lockheed Martin AdvancedTechnology Center)

218.11 – Photospheric and ChromosphericDynamics of Sunspots Observed with NewSolar TelescopeThe 1.6m New Solar Telescope (NST) of Big Bear SolarObservatory allows us to investigate the structure anddynamics of sunspots with unprecedented spatial andtemporal resolutions. We present results of simultaneousobservations of a sunspot in the photosphere with abroad-band TiO-line filter and in the chromospheric H-alphaline with Visible Imaging Spectrometer, and compare theobservational results with MHD models of sunspots. Theobservations reveal previously unresolved features of thesunspot umbra and penumbra. In particular, the TiO dataclearly demonstrate highly twisted dynamics of penumbralfilaments and umbral dots and reveal strong shearingplasma flows in sunspot bridges, not explained by the MHDsimulations. The high-resolution H-alpha spectroscopic dataprovide new views of the sunspot chromospheric dynamics,including the fine structure of oscillations and waves,penumbral jets, ubiquitous small-scale eruptions, andaccretion flows in a form of dense plasma sheets. Thediffraction-limited NST observations show that the sunspotdynamics is more complicated and much richer than it isdescribed by the current sunspot models.Author(s): Alexander Kosovichev (Crimean Astrophys.Observatory), Vasyl Yurchyshyn (New Jersey Institute of Technology)

218.12 – Structures of InterplanetaryMagnetic Flux Ropes and Comparison withTheir Solar SourcesWhether a magnetic flux rope is pre-existing or in-situformed in the Sun's atmosphere, there is little doubt thatmagnetic reconnection is essential to release the flux ropeduring its ejection. During this process, the questionremains: whether and how does the magnetic reconnectionchange the flux rope structure? In this work, we continuewith the original study by Qiu et al. (2007) by using a largersample (19) of events to compare properties of ICME/MCflux ropes measured at 1 AU and properties of associatedsignatures (flares, CMEs, filaments) on the Sun. Inparticular, the magnetic field-line twist distribution withininterplanetary magnetic flux ropes is systematically derivedand examined. The analysis results show that these fluxropes exhibit either a rather flat twist distribution fromcenter to edge or a high twist at the core which decreasestoward the edge. We also present detailed case studies forselected events with the corresponding solar source regionseither or not dominated by erupting filaments, and discusshow reconnection properties reflected in the flaremorphology may be related to the structure of the enfantflux rope formed on the Sun.Author(s): Jiong Qiu (Montana State University), Qiang Hu(University of Alabama in Huntsville)

218.13 – Fitting medium and high degreesusing GONG, MDI and HMI observations.I present results from fitting data from the three majorhelioseismic instruments: GONG, MDI, and HMI, both atmedium degree (resolved modes) and at high degrees(ridge fitting). The medium-l fitting was carried out ontime-series of varying lengths (1x, 2x, 4x, 8x, 16x, 32x, 64x72 day longs, and 36 day long ones), the high-l fitting wascarried out on co-eval time-series that correspond to the2001, 2002 and 2010 MDI Dynamics runs. I present theseresults, compare them and discuss the potential sources ofthe discrepancies.Author(s): Sylvain Korzennik (Harvard-Smithsonian, CfA)

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218.14 – Height-dependent Refraction of AGlobal EUV Wave and Its AssociatedSympathetic EruptionsThe height dependence of global extreme-ultraviolet (EUV)waves in the solar corona, especially of their wave-likebehaviors such as transmission and reflection, is critical tounderstanding their physical nature. Prior observations ofsuch behaviors, when detected on the solar disk, werecompromised because height-dependent information is lostdue to the line-of-sight projection from a top-down view. Wereport a global EUV wave on the limb observed by SDO/AIAfrom a side-view that evidently shows height-dependenttransmission and refraction. As the wave travels through anactive region, the orientation of the low-corona wave frontchanges from a forward inclination toward the solar surfaceto a backward inclination. This indicates that the EUV wavespeed is lower at higher altitudes, which is expectedbecause of the rapid drop with height of the Alfven andfast-mode speeds in active regions, as predicted by MHDmodels. When traveling into the active region, the EUVwave speed in the low corona increases from ~600 km/s to~900 km/s. In addition, in the neighborhood of the activeregion, sympathetic eruptions of local coronal structurestake place sequentially upon the wave impact and mayappear as wave reflection. Understanding propagationbehaviors of global EUV waves brings us one step closer tofully utilizing them for seismological diagnostics of theglobal corona, such as mapping the spatial distribution ofthe Alfven speed and magnetic field strength.Author(s): Wei Liu (Lockheed Martin Solar and AstrophysicsLaboratory), Leon Ofman (Catholic University of America and NASAGoddard Space Flight Center), Cooper Downs (Predictive Science Inc.),Karel Schrijver (Lockheed Martin Solar and Astrophysics Laboratory)

218.15 – A Helioseismic Survey toInvestigate Relationships betweenSubsurface Flows beneath Large ActiveRegions and Solar FlaresA survey of the subsurface flow properties of about 120 ofthe largest active regions, determined from the applicationof helioseismic holography to Dopplergrams obtained withthe HMI instrument onboard the Solar DynamicsObservatory, is being carried out. The overriding goal is tocharacterize differences in the subsurface flows betweenactive regions associated with eruptive flares and the flowsobserved in relatively quiescent regions. Applications toflare forecasting comprise only one part of thisinvestigation, since the potential response of thesubsurface environment to eruptive events during and aftertheir occurrence is also of scientific interest. Other prioritiesinclude understanding the limitations of the helioseismicmethods, identifying and correcting systematic effects, andvalidating the reliability of the measurements usingartificial data. While inversions to determine the variationwith depth of subsurface flows are planned, preliminaryresults will be discussed which make use of proxies fornear-surface depth-integrated properties, including thehorizontal component of the flow divergence and thevertical component of the flow vorticity. This work issupported by the Solar Terrestrial Program of the NationalScience Foundation, through grant AGS-1127327, and bythe National Oceanic and Atmospheric Administration SBIRprogram.Author(s): Douglas Braun (NorthWest Research Associates, Inc.), KLeka (NorthWest Research Associates, Inc.), Graham Barnes (NorthWestResearch Associates, Inc.)

218.16 – Numerical Simulation of a SlowStreamer-Blowout CMEWe present a 3D numerical MHD simulation of the 2008 Jun2 gradual streamer blowout CME that had virtually noidentifiable low coronal signatures. We energize the field bysimple footpoint shearing along the source region's polarityinversion line and model the background solar windstructure using an ?2MK isothermal wind and a low-orderpotential field source surface representation of the CR2070synoptic magnetogram. Our results show that the CME``initiation’’ is obtained by slowly disrupting the quasi-steady-state configuration of the helmet streamer, resultingin the standard eruptive flare picture that ejects thesheared fields, but very slowly, on a relatively large scale,and with very little magnetic energy release. We obtain arelatively slow CME eruption of order the background solarwind speed and argue that these slow streamer blowoutCMEs (now also known as ``stealth CMEs’’) are simply atthe lowest end of the CME energy distribution. We presentcomparisons of the CME propagation through the corona(?15Rs) in synthetic white-light images derived from thesimulation density structure with multi-spacecraftcoronagraph data from STEREO/SECCHI and SOHO/LASCO.Author(s): Benjamin Lynch (Univ. of California-Berkeley), SophieMasson (Goddard Space Flight Center), Yan Li (Univ. of California-Berkeley),C. DeVore (Goddard Space Flight Center), Janet Luhmann (Univ. ofCalifornia-Berkeley), Spiro Antiochos (Goddard Space Flight Center)

218.17 – Helioseismic Ring-diagramDiagnostics of Solar Fares.Flares are known to excite waves in the solar atmosphere.Maurya et al. (2009), using a local analysis (ring diagrams)of the 2003 Halloween flare, also showed they excitep-modes. We confirm and extend here these results by:-applying the same analysis to other locations on the Sunat the time of the Halloween flare -analyzing another eventalso showing a signature of p-mode excitation -looking indetails at the results of the ring diagrams analysis in termsof noise fitting. The Halloween flare present an apparentlocalized excitation of p-modes, similar to what is observedfor the other event analyzed.Author(s): John Leibacher (Institut d'Astrophysique Spatiale),Frédéric Baudin (Institut d'Astrophysique Spatiale)

218.18 – Active region 11748: RecurringX-class flares, large scale dimmings andwaves.AR 11748 was a relatively compact active region thatcrossed the solar disk between 05/14/2013 and05/26/2013. Despite its size it produced a number X-classflares, and global scale eruptive events that were capturedby the SDO Feature Finding Team's (FFT) Dimming RegionDetector. Using the results of this module and other FFTmodules, we present an analysis of the this AR region andinvestigate why it was so globally impactful.Author(s): Alisdair Davey (SAO), Anna Malanushenko (Lockheed MartinAdvanced Technology Center), Scott McIntosh (High Altitude Observatory)

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218.19 – Evolution of the Near-surfaceFlows Inferred from High-resolutionRing-diagram Analysis of HMI DataRing-diagram analysis of acoustic waves observed at thephotosphere provides in principle a relatively robustdetermination of the sub-surface flows at a particular timeunder a particular region. The depth of penetration of thewaves is related to the size of the region, hence the depthextent of the measured flows is inversely proportional tothe spatial resolution. Most ring-analysis has focused onregions of extent ~15 deg (200 Mm) or more in order toprovide reasonable mode sets for inversions. The HMIanalysis pipeline however also provides a set of ring fitparameters on a scale three times smaller. These provideflow estimates for the outer 1% (7 Mm) of the Sun only,with very limited depth resolution, but with spatialresolution adequate to map structures.potentiallyassociated with the belts and regions of magnetic activity.There are a number of systematic effects affecting thedetermination of flows from local helioseismic analysis ofregions over different parts of the observable disc, not allwell-understood. In this study we characterize thosesystematic effects with higher spatial resolution. Thisenable us to remove them more effectively as we map thetemporal and spatial evolution of the flows, leaving openthe question of their mean structure which is most affectedby the systematics. We present results for the ring-diagramdetermination of the flow anomalies corresponding to thetorsional oscillation pattern in differential rotation andanalogous patterns in the meridional cell structure over theearly part of the current solar cycle observed by HMI.Author(s): Richard Bogart (Stanford University), Charles Baldner(Stanford University), Sarbani Basu (Yale University)

218.20 – Structure and Dynamics of OnePolar Crown Prominence EruptionWe will present the recent progress on the investigation ofthe polar crown prominence that erupted on 2012 March12. This prominence is viewed at the east limb by SDO/AIAand displays a quasi vertical-thread structure. BrightU-shape (horn-like) structure is observed surrounding theupper portion of the prominence before the eruption andbecomes more prominent during the eruption. Whenviewed on the disk, STEREO-B shows that this prominenceis composed of a series of vertical threads and displays aloop-like structure during the eruption. We focus on themagnetic support of the prominence by studying thestructure and dynamics of the prominence before andduring the eruption using observations from SDO, Hinode,and STEREO. We found that the transition from slow rise tofast rise phase is associated with magnetic reconnectionbelow rising prominence threads. We also constructed aseries of magnetic field models (including sheared arcademodel and twisted flux rope model) of the prominenceusing the “flux rope insertion method”, we will comparethem with observations in order to find the best-fit model.Our recent progress on the thermodynamics of the eruptingprominence will also be presented.Author(s): Yingna Su (Harvard-Smithsonian Center forAstrophysics), Adriaan Van Ballegooijen (Harvard-Smithsonian Center forAstrophysics), Patrick McCauley (Harvard-Smithsonian Center forAstrophysics), Kathy Reeves (Harvard-Smithsonian Center forAstrophysics), Edward DeLuca (Harvard-Smithsonian Center forAstrophysics), Haisheng Ji (Purple Mountain Observatory, CAS)

218.21 – Photospheric andsub-photospheric Flows in Active RegionsThe availability of continuous high-cadence and high-spatialresolution Dopplergrams allows us to study sub-surfacedynamics that may be further extended to exploreprecursors of the solar activity. Since p-mode power isabsorbed in high magnetic field regions, the helioseismicinferences in these regions are associated with large errors.In order to validate results, we use Dopplergrams from bothspace-borne (Helioseismic Magnetic Imager-HMI) andground-based (Global Oscillation Network Group-GONG)observations to infer horizontal flows in photospheric andsub-photospheric layers in and around several activeregions with different characteristics. The photosphericflows are calculated using local correlation tracking (LCT)method while ring-diagram analysis technique is used toinfer flows in the sub-photospheric regions. A detailedcomparison between flows in shear layer and photosphericlayer will be made in order to study similarities anddiscrepancies in these results.Author(s): Kiran Jain (National Solar Observatory), Rudolf Komm(National Solar Observatory), Sushanta Tripathy (National SolarObservatory), B. Ravindra (Indian Institute of Astrophysics), Frank Hill(National Solar Observatory)

218.22 – Column Densities of an EruptiveProminence over TimeWe present a series of column density measurements foran eruptive prominence. The eruption occurred on March12th, 2012, and observations were recorded by theAtmospheric Imaging Assembly (AIA) aboard the SolarDynamics Observatory. We estimate the backgroundemission to obtain an optical depth, which can be used toestimate the column density at all positions along theprominence. This is done every 30 minutes for 2 daysleading up to the eruption. The series of column densitymaps can then be used to estimate the total mass of theprominence as it evolves with time. Whether or not there issignificant mass loss or loading is an important constrainton the eruption mechanism. Our early work has found nosignificant change in the prominence mass over the twodays leading up to the eruption, but we are currentlyworking to reconcile a discrepancy between independentestimations made using AIA's 193, 211, and 335 Angstrompassbands. The results from this work will be presented.Author(s): Patrick McCauley (Smithsonian AstrophysicalObservatory), Edward DeLuca (Smithsonian Astrophysical Observatory),Yingna Su (Smithsonian Astrophysical Observatory)

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218.23 – Sub-surface Meridional FlowResults from MWO, GONG, and MDI duringSolar Cycle 23Time series of full-disk Dopplergrams were acquired at the60-Foot Solar tower of the Mount Wilson Observatory everyyear between 1987 and 2009. Analysis of this archiverevealed that the focal plane of the Tower did experience asmall amount of systematic rotation, which suggested thatthe alignment of the optics had changed slightly over theyears since its construction in 1907. This has caused someof the initial daily flow maps to possess a so-called“washing machine” effect similar to the pattern that wasseen in raw GONG flow maps. We have incorporated asystematic program of ring-diagram analysis in which wehave tracked the raw solar images using five differingassumed instrumental rotation rates. We have then goneon to compute synoptic maps of the horizontal flow vectorsat several different depths over much of Solar Cycle 23 inorder to study how such an instrumental rotation mightaffect both the zonal and meridional flows as functions oflatitude, depth, and time. We compare these results withGONG and MDI flow measurements to empiricallydetermine the regime within which the MWO results arereliable and extend our analysis into Solar Cycle 22.Author(s): Stephen Pinkerton (University of Southern California),Edward Rhodes (University of Southern California), Richard Bogart(Stanford University)

218.25 – Measuring The Solar Radius WithSDO/HMI and SDO/AIA During The VenusTransit Of 2012During the Venus transit of 2012, the side camera of HMI(Helioseismic and Magnetic Imager, on board SDO) tookimages in the continuum near 6173 A at a 3.75 secondcadence. By timing the crossings by the center of theplanet of the solar limb (based on the Venus obscuration ofthe solar disk), and by comparing the results with anephemeris, we can accurately estimate the solar radius.Here, this radius is defined as the inflection point of thelimb darkening function. We obtain a value at 1 AU of959.58". We further discuss estimates of the statistical andsystematic errors in this measurement (in particular therole of the PSF correction), and we apply the same methodto AIA 1600 and AIA 1700 images.Author(s): Sebastien Couvidat (Stanford Univ.), Rock Bush (StanfordUniv.)

218.27 – RHESSI/SAS Observations of theOptical Solar Limb Over a Full Solar CycleThe Solar Aspect System (SAS) of the RHESSI satellitemeasures the optical solar limb in the red continuum with acadence typically set at 16 samples/s in each of three linearCCD sensors. RHESSI has observed the Sun continuouslysince its launch in early 2002, and we have acquired aunique data set ranging over a full 11-year solar cycle andconsisting of about 3x10^10 single data points. Analyzingdata for an initial period in 2004, these measurements haveled to the most accurate oblateness measurement to date,8.01+-0.14 milli arcsec (Fivian et al., 2008), a valueconsistent with models predicting an oblateness fromsurface rotation. An excess oblateness term can beattributed to magnetic elements possibly located in theenhanced network. We have started to also studyphotometric properties of our data. Previous observationsof latitude-dependent brightness variations at the limb hadsuggested the presence of a polar temperature excess aslarge as 1.5 K. The RHESSI observations, made with arotating telescope in space, have great advantages in therejection of systematic errors in the very precisephotometry required for such an observation. Our newmeasurements of latitude-dependent brightness variationsat the limb lead to a quadrupolar term (a pole-to-equatortemperature variation) of the order of 0.1 K, an order ofmagnitude smaller than previously reported. We presentthe analysis of these unique data, an overview of someresults and we report on our progress as we apply ourdeveloped analysis method to the whole 12 years of data.Author(s): Martin Fivian (Space Sciences Lab/ UC Berkeley), HughHudson (Space Sciences Lab/ UC Berkeley)

218.28 – Combining Models, Theory andObservations to Reconstruct CME and ShockMorphology and Create an EmpiricalPrediction ModelThere are many factors that contribute to the evolution andpropagation of a Coronal Mass Ejection as well asassociated shock waves in the interplanetary space,including both the initial characteristics of the CME as wellas the physical quantities of the solar wind regime the CMEwill be encountering. No one data set contains enoughinformation to constrain these parameters, but bycombining a number of different data sets including in-situsolar wind measurements, remote sensing white light andEUV observations, numerical models and using atheoretical propagation model based on aerodynamic drag,the study of multiple events can lead to an empiricalprediction model for the arrival of both the CME ejecta andshock at the Earth. The more events that are studied themore accurate the results will be as the forces governingCME acceleration/deceleration are better understood.Author(s): Phillip Hess (George Mason University), Jie Zhang(George Mason University)

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218.29 – Statistical Constraints on Joy's LawUsing sunspot data from the observatories at Mt. Wilsonand Kodaikanal, active region tilt angles are analyzed fordifferent active region sizes and latitude bins. A number ofsimilarly-shaped statistical distributions were fitted to thedata using maximum likelihood estimation. In all cases, wefind that the statistical distribution best describing thenumber of active regions at a given tilt angle is a Laplace

distribution with the form (2?)-1*exp(-|x-?|/?), with 2° ? ? ?11°, and 10° ? ? ? 40°.Author(s): Ernest Amouzou (Montana State University), AndresMunoz-Jaramillo (Harvard-Smithsonian Center for Astrophysics), PetrusMartens (Harvard-Smithsonian Center for Astrophysics), Edward DeLuca(Harvard-Smithsonian Center for Astrophysics)

218.30 – Rolling Motions During SolarProminence Eruptions in AsymmetricMagnetic EnvironmentsPanasenco et al. [1] report observations of several CMEsthat display a rolling motion about the axis of the eruptingprominence. Murphy et al. [2] present simulations ofline-tied asymmetric magnetic reconnection that make afalsifiable prediction regarding the handedness of rollingmotions of flux ropes during solar eruptions. We will presentinitial results of our work to investigate this prediction. Todetermine the strength and any asymmetric properties ofthe magnetic field in the regions of interest in thephotosphere, we use magnetograms from HMI. We use AIAobservations to determine if there is any rolling motion and,if so, what handedness the rolling motions have. We thencompare the photospheric magnetic information with thehandedness information to determine if there is anyrelationship between the two. Finally, we will discussprospects for diagnosing rolling motions of eruptingprominence using off-limb IRIS observations. [1] O.Panasenco, S. Martin, A. D. Joshi, & N. Srivastava, J. Atmos.Sol.-Terr. Phys., 73, 1129 (2011) [2] N. A. Murphy, M. P.Miralles, C. L. Pope, J. C. Raymond, H. D. Winter, K. K.Reeves, D. B. Seaton, A. A. van Ballegooijen, & J. Lin, ApJ,751, 56 (2012)Author(s): Sean McKillop (Smithsonian AstrophysicalObservatory), Mari Paz Miralles (Smithsonian Astrophysical Observatory),Nicholas Murphy (Smithsonian Astrophysical Observatory), PatrickMcCauley (Smithsonian Astrophysical Observatory)

218.31 – Temporal Variation of PhotosphericSpectral Lines Profiles with the Solar Cycleof ActivityWe investigated the variations in the sun-as-a-star profilesof several photospheric spectral lines observed during thedecline of solar cycle 23 and the rising phase of cycle 24.Daily measurements were taken with the IntegratedSunlight Spectrometer (ISS) operating at the National SolarObservatory at Kitt Peak (Arizona) since December 2006.ISS, which is one of three instruments comprising the SolarOptical Investigations of the Sun (SOLIS) facility, isdesigned to obtain high spectral resolution (R = 300,000)observations of the Sun as a star in a broad range ofwavelengths (350 nm - 1100 nm). Recent improvements inthe spectral calibration of SOLIS/ISS measurements havesignificantly enhanced the diagnostic capabilities of thesedata. We will present time series of line parameters anddiscuss their correlation to the global magnetic flux.Because of their different response to variations in thethermodynamic and magnetic structures of the solaratmosphere, the measured line shape parameters providean excellent tool to disentangle thermal and magneticeffects occurring during different phases of the solar cycle.The results of this analysis may also help with developing abetter understanding of magnetic cycle of activity in othersolar-like stars.Author(s): Luca Bertello (National Solar Observatory), AlexeiPevtsov (National Solar Observatory), Andrew Marble (National SolarObservatory)

218.32 – Some analysis based on three flareassociated CMEsMagnetic reconnection is the main energy release processduring a solar eruption. We try to investigate therelationship between CMEs and magnetic reconnection byanalyzing three flare associated CMEs observed by STEREOand SDO. We focus on tracking CMEs from surface andcomparing them with associated flare evolutions. We alsocompare our results with the numerical work.Author(s): Jianxia Cheng (Shanghai Astronomical Observatory,CAS), Jiong Qiu (Montana State University), Shane Sullivan (NorthernIllinois University)

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218.33 – The Constant Size and Shape ofthe SunOver the last four years, the Helioseismic and MagneticImager (HMI) instrument on the Solar DynamicsObservatory spacecraft has been measuring the radius andoblateness of the Sun. The primary observations for thesolar radius are full Sun images taken twice per day in thecontinuum wing of the 617.3 nm Fe I absorption line. Thesolar radius is defined as the mean distance from thecenter of the Sun to the inflection point of the limbdarkening function. After correcting for the varyingSun-spacecraft distance and temperature variation of theoptics, the measured solar radius is essentially constantover the rising phase of the solar cycle. Measurements ofthe solar oblateness are obtained twice per year in Apriland October when the spacecraft is rotated 360 degreesaround the Sun-spacecraft line. HMI observations takenduring these roll maneuvers allow the instrument distortionto be separated from the solar shape. There is an apparentspring to fall change which may be due to seasonalvariation of the measurements which have not beencorrected. The long term trend of the solar oblateness,however, does not show a correlation with the current solarsunspot cycle.Author(s): Rock Bush (Stanford University), Marcelo Emilio(Universidade Estadual de Ponta Grossa), Jeffrey Kuhn (University ofHawaii)

218.34 – Comparison of CME three-dimensional parameters derived from singleand multi-spacecraftSeveral geometrical models (e.g., cone and flux ropemodels) have been suggested to infer three-dimensionalparameters of CMEs using multi-view observations(STEREO/SECCHI) and single-view observations(SOHO/LASCO). To prepare for when only single viewobservations are available, we have made a test whetherthe cone model parameters from single-view observationsare consistent with those from multi-view ones. For thistest, we select 35 CMEs which are identified as CMEs,whose angular widths are larger than 180 degrees, by onespacecraft and as limb CMEs by the other ones. For this weuse SOHO/LASCO and STEREO/SECCHI data during theperiod from 2010 December to 2011 July when twospacecraft were separated by 90±10 degrees. In this study,we compare the 3-D parameters of these CMEs from threedifferent methods: (1) a triangulation method usingSTEREO/SECCHI and SOHO/LASCO data, (2) a GraduatedCylindrical Shell (GCS) flux rope model usingSTEREO/SECCHI data, and (3) an ice cream cone modelusing SOHO/LASCO data. The parameters used forcomparison are radial velocities, angular widths and sourcelocation (angle ? between the propagation direction and theplan of the sky). We find that the radial velocities and the?-values from three methods are well correlated with oneanother (CC > 0.8). However, angular widths from the threemethods are somewhat different with the correlationcoefficients of CC > 0.4. We also find that the correlationcoefficients between the locations from the three methodsand the active region locations are larger than 0.9, implyingthat most of the CMEs are radially ejected.Author(s): Harim LEE (Kyung Hee University), Yong-Jae Moon (KyungHee University), Hyeonock Na (Kyung Hee University), Soojeong Jang(Kyung Hee University)

218.35 – Which CME cone type is closer toobservations?Recently, CME cone models are widely used for inferringthree dimensional structures of CMEs and their propagationthrough the heliosphere, especially for the inputparameters of CME propagation models. However, therehas been no observational test which cone type is closer toobservations. In this study, we investigate which conemodel is proper for halo CME morphology using 33 CMEswhich are identified as halo CMEs by one spacecraft and aslimb CMEs by the other ones. These CMEs were taken bySOHO/LASCO and STEREO/SECCHI during the period from2010 December to 2011 June when two spacecraft wereseparated by 90±10 degrees, which allow us to directlyestimate their angular widths from observations. Fromgeometrical parameters of these CMEs such as their frontcurvature, they are classified into two groups: shallow coneCMEs (5 events), whose curvature radius is equal to thedistance of CME front from the center of the Sun, and nearfull-cone CMEs (28 events), whose front has a semi-circleshape. Noting that the previous cone models are based onflat cone or shallow cone shapes, our results imply that acone model based on the full cone shape should bedeveloped.Author(s): Hyeonock Na (Kyung Hee University), Soojeong Jang(Kyung Hee University), Jea-Ok Lee (Kyung Hee University), Harim LEE(Kyung Hee University), Yong-Jae Moon (Kyung Hee University)

218.36 – Temperature and mass estimationof erupting plasma associated with coronalmass ejections observed by Hinode/XRT andSDO/AIAWe investigate the temperature and mass of eruptingplasma observed in X-ray and EUV, which are associatedwith coronal mass ejections (CMEs) and X-class flares.Hinode/XRT observed the erupting hot plasma in a fewpassbands, which allows us to determine the temperatureof the plasma using a filter ratio method. SDO/AIA observedthe erupting plasma in EUV passbands. We estimate thetemperatures and emission measures of the eruptingplasma in EUV using a differential emission measuremethod. One of these observations shows an eruptiveplasma with a loop-like structure in X-ray and EUV. Thetemperature of the erupting plasma in X-ray is about 13 MKby the filter ratio method. The estimated mass of thiserupting plasma in X-ray is similar to that in EUV. A coupleof events are associated with the eruptions of prominencesas absorption features in EUV in addition to hot plasmaeruption. One event shows that the absorption featureschange to emission features at the beginning of theireruptions in all EUV wavelengths of SDO/AIA. By estimatingthe temperature and mass of the erupting plasmas, wediscuss the heating of the plasmas associated with coronalmass ejections in the low corona.Author(s): Jin-Yi Lee (Kyung Hee University), John Raymond (Harvard-Smithsonian Center for Astrophysics), Kathy Reeves (Harvard-SmithsonianCenter for Astrophysics), Yong-Jae Moon (Kyung Hee University), Kap-SungKim (Kyung Hee University)

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218.37 – The Role of CMEs in the Escape ofSolar Energetic ParticlesHeliospheric manifestations of intense energy releaselinked to solar activity include the impact at Earth ofenergetic particles accelerated during solar eruptions.Observationally, the magnetic configuration of activeregions, where solar eruptions occur, agrees well with thestandard model of eruption, consisting of a flare and acoronal mass ejection (CME). According to the standardmodel, particles accelerated at the flare reconnection siteshould remain trapped in the CME. However, flare-accelerated particles frequently reach the Earth long beforethe CME does. We present a 3D model that demonstrateshow flare-accelerated particles escape into interplanetarymagnetic flux tubes during a solar eruption. Our model isbased on results of large-scale 3D MHD simulations of abreakout CME erupting into a heliospheric magnetic fieldthat is opened by an isothermal solar wind. The simulationsare performed with the Adaptively Refined MHD Solver(ARMS). We describe the multiple reconnection episodesthat occur during the evolution of the event, and show howCME magnetic flux reconnects with the open field from anearby coronal hole. This reconnection allows flare-accelerated particles initially trapped in the CME to escapeonto open field lines. Analyzing the dynamics of thereconnected flux during the eruption, we determine thespatial distribution of particle beams originating in the CMEflux rope. We find that particle release can occur over awide longitudinal range, which heretofore has been apuzzling feature of SEP observations. We discuss theimplications of our results for CME/flare models and for theorigin and transport of SEPs. This work was supported, inpart, by the NASA TR&T and SR&T Programs.Author(s): Sophie Masson (NASA/GSFC), Spiro Antiochos(NASA/GSFC), C. DeVore (NASA/GSFC)

218.38 – Results from Persistence Mappingof Solar EUV DataPersistence Mapping is a simple image processingtechnique that is useful for the visualization and depictionof gradually evolving or intermittent structures. PersistenceMapping allows the user to isolate extreme values in a dataset, and is particularly useful for the problem of capturingphenomena that are evolving in both space and time. Whileintegration or "time lapse" imaging uses the full sample (ofsize N), Persistence Mapping rejects (N-1)/N of the data setand identifies the most relevant 1/N values using thefollowing rule: if a pixel reaches an extreme value, it retainsthat value until that value is exceeded. The simplestexamples isolate minima and maxima, and the techniquehas been used to extract the dynamics in long-termevolution of comet tails, erupting material, spicules, andEUV dimming regions. The presentation will review thetechnique and discuss scientific results obtained throughPersistence Mapping. For more information, please seehttp://sipwork.org/persistence-mappingAuthor(s): Barbara Thompson (NASA's GSFC), C. Young (NASA'sGSFC)

218.39 – SunPy - Python for Solar Physics,Version 0.4We presents version 0.4 of SunPy, a community-developedPython package for solar physics. Python, a free, cross-platform, general-purpose, high-level programminglanguage, has seen widespread adoption among thescientific community, resulting in the availability of a largenumber of software packages, from numerical computationNumPy, SciPy and machine learning (scikit-learn) tovisualisation and plotting (matplotlib).SunPy is adata-analysis environment specialising in providing thesoftware necessary to analyse solar and heliosphericdatasets in Python. SunPy is open-source software (BSDlicence) and has an open and transparent developmentworkflow that anyone can contribute to. SunPy providesaccess to solar data through integration with the VirtualSolar Observatory (VSO), the Heliophysics EventKnowledgebase (HEK), and the HELiophysics IntegratedObservatory (HELIO) webservices. It currently supportsimage data from major solar missions (e.g., SDO, SOHO,STEREO, and IRIS), time-series data from missions such asGOES, SDO/EVE, and PROBA2/LYRA, and radio spectra frome-Callisto and STEREO/SWAVES. We describe SunPy'sfunctionality, provide examples of solar data analysis inSunPy, and show how Python-based solar data-analysis canleverage the many existing tools already available inPython. We discuss the future goals of the project andencourage interested users to become involved in theplanning and development of SunPy.Author(s): Steven Christe (NASA GSFC), Stuart Mumford (University ofSheffield), David Perez-Suarez (South African National Space Agency -Space Science), Jack Ireland (ADNET systems), Albert Shih (NASA GSFC),Andrew Inglis (Catholic University), Simon Liedtke (University of Bremen),Russel Hewett (MIT)

Contributing teams: Sunpy collaboration

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218.40 – Naming Collections of SolarPhysics DataTo better deal with tracking cross-discipline data usage, anumber of groups have come up with guidelines andprinciples for data citation. In 2012, the National Academy'sBoard on Research Data and Information released thereport "For Attribution-Developing Data Attribution andCitation Practices and Standards" [1] and it was followedlast year by the CODATA-ICSTI report "Out of Cite, Out ofMind".[2] Participants from a number of groups synthesizeda single set of principles for data citation that could beendorsed by all groups involved in research.[3]Implementing these principles can help to improve thescientific ecosystem by giving proper attribution to allcontributors to data, improving transparency andreproducability, and making data more easily reusable toboth astronomers and other researchers. Unfortunately, toimplement these principles, we first need to come up withappropriate groupings of data such that they can be easilycited.[4] From this, we can determine appropriatenames/titles to unambiguously identify them. The VirtualSolar Observatory will need to work with PI teams todetermine these groupings and document them using theDataCite schema.[5] We will present the Joint Declaration ofData Citation Principles and the DataCite schema, discussthe implication of them for solar physics data, andrecommend steps towards implementation. References: [1]National Research Council, 2012. http://www.nap.edu/catalog.php?record_id=13564 [2] CODATA, 2013.http://dx.doi.org/10.2481/dsj.OSOM13-043 [3] FORCE11,2014. http://www.force11.org/datacitation [4] Wynholds,2011. http://dx.doi.org/10.2218/ijdc.v6i1.183 [5] DataCite,2013. http://dx.doi.org/10.5438/0008Author(s): Joseph Hourcle (Wyle IS)

Contributing teams: Virtual Solar Observatory, FORCE11Data Citation Synthesis Group

218.41 – Final (or Maybe Not So Final)Archiving of Solar Physics Data: Assuringthe Validity of and Access to Data in thePost-NSSDC EpochHistorically, NASA's National Space Science Data Centerwas responsible for the long-term preservation, periodicrevalidation and recording medium transfer of, and accessto, older space solar physics data sets. The NSSDC is fadingfrom view, however, and the Heliophysics DataManagement Policy calls for discipline-specific “finalarchives,” where “final” somehow means less final than a“long-term archive.” The Solar Data Analysis Center may betasked with the “final” archiving of space solar physics datasets, but we have no expertise in the data preservationactivities traditionally carried out by the NSSDC. We alsorecognize that the largest space solar physics data set, theSDO AIA and HMI data at the Stanford Joint Science andOperations Center (JSOC), will also need preservation andlong-term access, as will the potentially much larger dataarchive of DKIST observations. We have therefore begun astudy of data archiving best practices in other disciplinesand organizations, including NASA’s Space Physics DataFacility (SPDF), the National Institute of Standard andTechnology (NIST), and private industry. We report on thelessons learned so far, and possible cost models. We seekinput from the broader solar physics community on therelative value of various levels of preservation effort.Author(s): Joseph Gurman (NASA GSFC), Jennifer Spencer (NASA GSFC)

218.42 – The Availability of Higher LevelSDO/HMI Data ProductsThe Solar Dynamics Observatory Helioseismic and MagneticImager (SDO/HMI) investigation proposed to generate a setof "high level" data products. These are data products thatrequire processing and analysis well beyond the traditionalproducts prepared by Heliophysics mission teams. That is,these are not simply images nor what the HMI team calls"Observables" which are e.g. magnetograms orDopplergrams. The traditional deliverd data products areoften referred to as "Level-1" data products and are thehighest level of processing required by contract with NASA.The HMI team planned to also produce higher levelproducts such as flows in the solar interior, solar oscillationmode frequencies and inversions for interior rotation,magnetic vector field inversions with disambiguation,derived indices that may have space-weather applications,et cetera. Most of these products are now in regularproduction and a series of recent papers and papers inprogress describe them in detail. This poster is to bringattention to the availability of these products and describewhere and how to get the needed information to use themfor new research objectives.Author(s): Philip Scherrer (Stanford Univ.)

Contributing teams: SDO/HMI Science Team

218.43 – Challenges for the DKIST DataCenterProcessing the large volumes of complex, multi-instrument,ground-based data generated at the DKIST will requireimplementation of algorithms and tools at a level notpreviously achieved for high-resolution, ground-based solartelescopes. We discuss some the goals of the datareduction pipelines for DKIST, including the different typesof calibrations that would (optimally) be applied to theacquired data. We highlight some of the particularchallenges for ground-based data, including seeing effects,atmospheric dispersion, and rapid changes in instrumentalcalibrations. We will describe a possible softwareframework for the implementation of the pipelines, as wellas point out some areas for community input or VSOintegration in the development process.Author(s): Kevin Reardon (National Solar Observatory), ThomasRimmele (National Solar Observatory)

218.44 – Helioviewer.org: Enhanced Solar &Heliospheric Data VisualizationHelioviewer.org enables the simultaneous exploration ofmultiple heterogeneous solar data sets. In the latestiteration of this open-source web application, TRACE andHinode XRT join SDO, SOHO, STEREO, PROBA2 SWAP, andYohkoh SXT as supported data sets, with significantadditions to the availability of data from STEREO. Version 2of Helioviewer's Public API for scientists and softwaredevelopers provides powerful new ways to interact withsolar data, complete with extensive documentation andusage examples. A new data coverage visualizationdemystifies the availability of each data set. The addition ofa science data download tool provides a simple way toimport FITS files directly into an IDL or Python analysisenvironment. Finally, a prototype timeline feature exploresnew ways of browsing image data sets in our viewport aswell as interacting with time series data.Author(s): Jeffrey Stys (ADNET Systems Inc.), Jack Ireland (ADNETSystems Inc.), V. Hughitt (ADNET Systems Inc.), Daniel Mueller (EuropeanSpace Agency)

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218.45 – WIMAGR: An Interactive SSW IDLTool for Mapping OVSA Legacy MicrowaveInterferometry DataThe Owens Valley Solar Array (OVSA), which is currently thesubject of a major upgrade leading to the new ExpandedOwens Valley Solar Array (EOVSA), has operated betweenthe years 2000-2007 as a 5-7 antenna solar-dedicated radiointerferometer, with daily observations at typically 40frequencies in the microwave frequency range, 1-18 GHz.Given the importance of these unique data forcomplementary studies with data taken during the sameperiod by Yohkoh, RHESSI, SoHO, TRACE, Hinode and otherNASA spacecraft, we have undertaken an effort tomaximize their usefulness, ease of use, and longevity bycreating a uniform, calibrated OVSA legacy database andcommunity-friendly, SSW-based software, compatible withthe RHESSI and EOVSA software packages. With theseefforts, we can anticipate that the data will continueserving the community well into the future. In thispresentation, we will introduce one of the recent upgradesof the OVSA SSW software package, WIMAGR, whoseinterface allows the user to generate OVSA radio maps inintensity and polarization at many available frequencieswith a spatial resolution about 3” at 18 GHz, which iscomparable with the spatial resolution of other imaginginstruments. To illustrate the main capabilities of thissoftware tool and its potential for promoting scientificdiscovery, we will present a real-time computation of asequence of multi-frequency OVSA microwave maps andcompare them with images obtained by other instruments.This work was supported in part by NSF grantsAGS-1250374, and NASA grants NNX11AB49G andNNX14AC87G to New Jersey Institute of TechnologyAuthor(s): Gelu Nita (NJIT), Gregory Fleishman (NJIT), Dale Gary (NJIT)

218.46 – The Virtual Solar Observatory: NewData, Big Data and Better QueriesThe Virtual Solar Observatory (VSO) is entering its seconddecade of serving data to the solar physics community. Itcontinues to provide 'homogenous access to heterogeneousdata' at ever increasing volumes, thanks primarily to theSolar Dynamics Observatory. In 2013, the SmithsonianAstrophysical Observatory, one of the primary VSO sites forSDO data distribution served over 90TB in user requestsalone. Despite SDOs dominance in terms of data volume,we continue to make available new data sets, and updateand improve access to current ones especially via the IDLinterface to the VSO. Here we detail new data sets, giveupdates on new querying capabilities and preview what liesahead for VSO.Author(s): Alisdair Davey (SAO)

Contributing teams: The Virtual Solar Observatory Team

218.47 – Rapid Multi-Scale Decompositionof Solar ImagesMulti-scale decomposition of astronomical images has beencodified into several processing routines in a wide range ofimage types. This type of decomposition uses band-passfiltering to isolate features of a specific scale from theoriginal data. At each scale, it is then possible to estimateand subtract a noise contribution and amplify a desiredsignal. We apply this approach to time series ofhigh-resolution solar images. Using a multi-scale analysis ofsolar images coupled with a high time cadence, we are ableto extract an evolving noise estimate as the solarenvironment changes.Author(s): Michael Kirk (NASA), C. Young (NASA)

218.48 – Standardizing Documentation ofFITS HeadersAlthough the FITS file format[1] can be self-documenting,human intervention is often needed to read the headers towrite the necessary transformations to make a giveninstrument team's data compatible with our preferredanalysis package. External documentation may be neededto determine what the values are of coded values orunfamiliar acronyms. Different communities haveinterpreted keywords slightly differently. This has resultedin ambiguous fields such as DATE-OBS, which could beeither the start or mid-point of an observation.[2]Conventions for placing units and additional informationwithin the comments of a FITS card exist, but they requirere-writing the FITS file. This operation can be quite costlyfor large archives, and should not be taken lightly whendealing with issues of digital preservation. We present whatwe believe is needed for a machine-actionable external filedescribing a given collection of FITS files. We seekcomments from data producers, archives, and those writingsoftware to help develop a single, useful, implementablestandard. References: [1] Pence, et.al. 2010,http://dx.doi.org/10.1051/0004-6361/201015362 [2] Rots,et.al, (in preparation), http://hea-www.cfa.harvard.edu/~arots/TimeWCS/Author(s): Joseph Hourcle (Wyle IS)

Contributing teams: Virtual Solar Observatory

218.49 – Using FLCT to Obtain SpectralInformation From MOSES DataThe Multi-Order Solar EUV Spectrograph (MOSES) is a highcadence slitless spectrograph that images in He II 304Å.The large field of view (20’x10’) combined with the abilityto quickly obtain images containing both spectral andspatial information makes MOSES an ideal platform forprobing small scale, short duration flows resulting frommagnetic reconnection in the solar transition region. Theease of obtaining co-temporal spectral and spatial datawith a slitless spectrograph is counterbalanced byincreased difficulty required to disentangling theinformation captured in the images. The Fourier LocalCorrelation Tracking (FLCT) routine developed by Fischerand Welch (2007) is developed as a technique for obtainingDoppler shifts and line widths from small scale flowsimaged by MOSES. Results are reported utilizing thistechnique on simulated images and MOSES data.Author(s): Hans Courrier (Montana State University), CharlesKankelborg (Montana State University)

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219 – Variable Stars, Binaries, and Compact Objects PostersPoster Session – Essex Ballroom and America Foyer – 03 Jun 2014 09:00 AM to 06:30 PM

219.01 – Variable Stars from the MG-1CatalogThis work describes the recent efforts at North CarolinaA&T(NCAT) mining the MG catalogs for variable stars. NCATis a node in both the GNAT network and the SKYNETcollaboration which forms the basis of the collaborationincluding access to instruments. The initial data analysis toobtain the light curves (LC) for MG-1 has been performedand a number of candidate variable stars have beenidentified including brown dwarf stars, eclipsing binariesand long period variable stars. Many of the identifiedcandidate variable stars are now the subject of coordinatedmulti-site follow-on observations to elucidate the details ofthe variability. The coordinated observing includesresearchers in Australia, Arizona, Colorado and NorthCarolina. As a node in both the GNAT network and theSKYNET collaboration NCAT has access to a number ofinstruments. Much of the observational work is performedusing the SKYNET node in Chile. For the North Carolina workreported here, the observational work and initial LCgeneration is performed using telescopes and applicationsfrom the SKYNET program. In this work the instrumentation,the LC analysis and status of the coordinated follow-onobservations are presented.Author(s): K. M. Flurchick (North Carolina AandT State University),Ben Griego (North Carolina AandT State University), Roger Culver(Colorado State University)

219.02 – The UM-Dearborn Observatory:Variable-object Research from an UrbanSiteSince its construction in 2007, the UM-DearbornObservatory has provided a valuable educational tool bothfor students at UM-Dearborn and our neighbor-institutionthe Henry Ford Community College, and for the publicat-large. We have recently (Jan 2014) added a systematiclong-term research program with our 0.4m main telescope,to photometrically monitor a number of bright variableobjects, including X-ray binaries and chemically-peculiarmetal-poor stars over long timescales. We ultimatelyenvision assembling a photometric database of (at least)four-color photometry over years-decades (i.e., manyhundreds of orbital timescales for close binaries), with thepreponderance of datapoints taken by undergraduates. Toconduct this program, we have had to overcome a numberof site challenges, the solutions of which will be useful tomany programs using small telescopes at urban sites. The0.4m telescope lies on a shared building withinUM-Dearborn's main Fairlane campus - i.e., is about 20meters above sea level, near several sources of watervapor (including an active steam vent less than 15 metersaway), experiences significant mechanical vibrations fromother building functions, and lies about 6 miles from centralDetroit, well within the Detroit-Ann Arbor conurbation.Observing conditions are thus highly variable, with 5arcsecond seeing typical and significant transparencyvariations observed even during a clear night.Nevertheless, we are now able to make scientifically usefulobservations in a semi-automatic way, to which our chosenscientific niche is well-suited. We present here our solutionsto these challenges, along with initial results from ourongoing monitoring program.Author(s): Elisabeth Clyne (University of Michigan-Dearborn),William Clarkson (University of Michigan-Dearborn), Eric Rasmussen(University of Michigan-Dearborn), Donald Bord (University of Michigan-Dearborn), Kristen Dage (University of Michigan-Dearborn), David Matzke(University of Michigan-Dearborn), Carrie Swift (University of Michigan-Dearborn)

219.03 – Variability in Hot Subdwarfs andRelated Objects from the Palomar-GreenCatalogWe present a selection of objects chosen from thePalomar-Green (PG) Catalog of Ultraviolet Excess StellarObjects to search for variability. Variability could be fromeclipsing binaries, cataclysmic variables, the irradiationeffect and many others. The PG catalog used the Palomar18 inch telescope to look for stars that were brighter in theultraviolet than normal stars. One result of the PG catalogwas a discovery of hot subdwarfs (sd) that dominated thesky. We chose 988 stars because they were classified in thePG catalog as sd stars or as related objects and present ananalysis of 475. We used the Catalina Real-Time TransientSurvey and the UBVRI photometric standard stars fromLandolt to find that approximately 60 of these objects showevidence of being variable.Author(s): Melissa Blacketer (California State University, Fresno),Fred Ringwald (California State University, Fresno)

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219.04 – The Semiregular Variable StarObserving Program at Grinnell CollegeA large body of photometric and spectroscopic data on 38semiregular variable stars has been acquired at the GrantO. Gale Observatory of Grinnell College since 1984. Thisincludes V and B band photoelectric photometry, CCDspectroscopic monitoring, and a large set of spectra for RSCygni. The stars in the program were selected becausethey had a history of “quiescent episodes” in theirpulsations that might be explained as mode switches.Time-dependent Fourier analysis has been applied to thephotometric data to reveal the dominant frequencycomponents represented in the light curves and toinvestigate how the strengths of those components vary –sometimes quite abruptly – over time. The spectroscopicmonitoring of the entire set of stars is an ongoing project.The 413 RS Cygni spectra have been used to explore thevariation of spectral features with phase. The conspicuousdip near the peak of the RS Cygni light curve does notappear to be associated with obvious variations in thestrengths of spectral features.Author(s): Robert Cadmus (Grinnell College)

219.05 – Photometry and Spectroscopy ofBD+35 1111 in M38BD+35 1111 is a ~10.5-magnitude star in the field of M38,an open cluster that has been a target of our ongoing studyof H? emission variability in massive stars via narrowbandCCD photometry (e.g. Souza, Davis, and Teich 2013, BAAS.45, PM354.22). BD+35 1111 has no MKK classification inthe literature, and is not listed as variable in GCVS, VSX, orNSVS. It is included, with no further characterization, inboth the Vatican and Kohoutek catalogs of emission linestars. Using inhomogeneous ensemble photometry (e.g.Bhatti, Richmond, Ford, and Petro 2010, ApJ Supp., 186,233), we find it to be an irregular variable with a range of~0.15 mag. To further understand this star we obtained amedium-resolution spectrum using the DIS spectrograph onthe ARC 3.5-meter telescope at Apache Point Observatory.We classify BD+35 1111 as B2Ve, the only confirmed Bestar in the field of M38. This raises the question ofmembership, since the age of M38 is likely 250 Ma orgreater (Pandey et al. 2007, Publ. Astron. Soc. Japan 59,547). From published B and V magnitudes we find anominal distance to BD+35 1111 of 1.6 kpc, but with arange of 1.3 to 2.0 kpc, marginally consistent with distanceestimates for M38 ranging from 1.0 to 1.4 kpc. If a member,BD+35 1111 is a candidate blue straggler. If not, it mayhave escaped from a nearby younger cluster, possiblyKronberger 1 (Kronberger et al. 2006, A&A 447, 921), whichhas the right heliocentric distance and age. The notion thatBD+35 1111 is behind M38 is supported by its reddening ofEB-V ~ 0.5, significantly higher than for M38 itself (~ 0.24).We gratefully acknowledge support for student researchfrom NSF grant AST-1005024 to the Keck NortheastAstronomy Consortium, Williams College, and NASA via anAmerican Astronomical Society Small Research Grant.Author(s): Steven Souza (Williams College), Karen Kwitter (WilliamsCollege), Mona Sami (Williams College), Gillian Beltz-Mohrmann (WellesleyCollege)

219.06 – The MOST Accurate Photometry forCepheid ModesFundamental mode classical Cepheids have famouslyrepeatable light curves and periods steady enough that wecan watch them evolve (change period). Overtonepulsators, on the other hand often have period changes toolarge to be explained by evolution, at least during thelongest (second and third) passages through the instabilitystrip. We obtained a month long series of observations withthe MOST satellite of the fundamental mode Cepheid RTAur and the first overtone pulsator SZ Tau. RT Aur showsthe traditional strict repetition of the light curve, with theFourier amplitude ratio R1/R2 remaining constant (varyingby only a percent). The light curve of SZ Tau, on the otherhand, fluctuates in amplitude ratio at the level ofapproximately 50\%. Furthermore prewhitening the RT Aurdata with 10 frequencies reduces the Fourier spectrum tonoise. For SZ Tau, considerable power is left after thisprewhitening in a complicated variety of frequencies.Financial Support was provided by CXC NASA ContractNAS8-03060 (NRE), ESTEC Contract No. 4000106398/12/NL/KML (LS), European Community's Seventh FrameworkProgramme (FP7/2007-2013) under Grant Agreement No.269194(IRSES/ASK) (RS, AD).Author(s): Nancy Evans (SAO), Robert Szabo (Konkoly Obs.), LaszloSzabados (Konkoly Obs.), Aliz Derekas (Konkoly Obs.), Laszlo Kiss (KonkolyObs.), Jaymie Matthews (Univ. British Columbia), Chris Cameron (Univ.British Columbia)

Contributing teams: The MOST Team

219.07 – Principle Component Analysis ofCepheid Variable StarsWe use Principle Component Analysis (PCA) and Fourierdecomposition on LMC and SMC cepheids observed byOGLE III to find relationships between a cepheid's period,luminosity, and light curve structure. Unlike the Period-Luminosity and Period-Luminosity-Color relations, these areindependent of extinction. We consider their advantagesand disadvantages in estimating distances.Author(s): Daniel Wysocki (SUNY Oswego), Zachariah Schrecengost(SUNY Oswego), Earl Bellinger (Indiana University), Shashi Kanbur (SUNYOswego), Sukanta Deb (Department of Physics, University of Delhi),Harinder Singh (Department of Physics, University of Delhi)

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219.08 – Photometric Analysis of theRecently Discovered W UMa Star NRCamelopardalis: Period Change and SpotMigrationNR Cam is a short period (P=0.26 days) eclipsing binary ofthe W UMa type that was relatively recently discovered inthe ROTSE1 data of the Northern Sky Variability Survey(NSVS) and was originally listed in the New Catalog ofSuspected Variable Stars (NSV) with the identifier NSV3754. Here we present the first known detailed study of NRCam, which includes multi-band light curves, color curves,and a photometric orbital solution. NR Cam exhibits astrong O'Connell effect that can be attributed tomagnetically induced spot activity on one of thecomponents. Absolute photometry was performed in B andV at the Kutztown University Observatory in 2013 Octoberand November and complementary high precisiondifferential light curves were obtained in BVRI at the sametime, as part of the KELT follow-up network, at BrighamYoung University's West Mountain Observatory, SwarthmoreCollege's Peter Van de Kamp Observatory, and theUniversity of Louisville's Moore Observatory. After the B-Vcolor curves were used to approximate the stellar surfacetemperatures and spot locations, the Wilson-Devinney codewas employed with a differential corrections routine todetermine the most likely stellar properties and orbitalparameters. Our solution indicates that the two stars are incontact, sharing a common envelope, and their surfacetemperatures are approximately 4500 K and 4200 K. Theinclination of the orbit was determined to be 68.0 (±0.6)degrees. When compared with the NSVS data, we find thatthe orbital period of NR Cam has changed over the pastdecade and that the strength of the O'Connell effect, andthe associated spot activity, has also varied significantly.Author(s): Jenae Shoup (Kutztown University), Phillip Reed (KutztownUniversity), Michael Joner (Brigham Young University), Eric Jensen(Swarthmore College), Karen Collins (University of Louisville), JoshuaPepper (Lehigh University)

219.09 – UBVRI Photometric Study of theTotally Eclipsing 6500 K Extreme Mass RatioW UMa Binary, GSC 3208 1986We present high precision, UBVRcIc light curves of thesuspected eclipsing binary, GSC 3208 1986. Theamplitudes of the light curve is very nearly 0.5 mag in allfilters. The present curves are immaculate with all spotactivity hidden within the low noise of the light curves. Theminima are equal to within 0.1 mags. The Wilson Devinneyprogram simultaneous light curve solution shows that thisis a totally eclipsing classic A-type, EW binary. GSC 32081986 is an extreme mass ratio, 6500 K, W UMa system. Themass ratio is only 0.24, with a component temperaturedifference of only ~100K. This points to a high degree ofthermal and physical contact. Indeed, the Roche lobefill-out is 39%. The high inclination of 85° results in a longduration secondary total eclipse (an interval of constantlight), some 49.5 minutes! The binary is of F6V type, andhas no modeled surface discontinuities (no spots wereneeded in the modeling). The period study of a 13 yeartime duration indicates that the period is steadilydecreasing. This is expected in solar type binariesundergoing magnetic braking. The variable is apparentlyundergoing solar-type activity with its associated magneticbreaking despite the near absence of spot distortions in thelight curves. However, an early curve by Gettel et al. (2006)may give evidence for this. All indications are that thisbinary is mature and approaching a transitionalcoalescence into a fast rotating A-type star (Guinan andBradstreet 1988).Author(s): Ronald Samec (Bob Jones Univ.), Danny Faulkner(University of South Carolina), Walter Van Hamme (Florida InternationalUniversity), James Kring (Bob Jones Univ.)

219.10 – Comparison of Observations andAnalyses of 2009 and 2012 Light Curves forthe Precontact W UMa Binary, V1001CassiopeiaA 2012 follow up to the analysis of 2009 observations ispresented for the very short period (~0.43d) precontactWUMa Binary, V1001 Cassiopeia. Its short period, similar tothe majority of W UMa’s, has a distinct EA light curve makeit a very rare and interesting system for continuingphotometric investigation. Previous photometric VRIstandard magnitudes give a K4 spectral type (Samec2012). Our solutions of light curves separated by some 3years give approximately the same physical parameters.However the spots have radically changed, bothtemperature, area and position wise. Whereas only onedark spot was used to model the first curves, two hot spotsare now needed. This affects the overall shape of the lightcurve, especially in the secondary eclipses in B and V.Additional eclipse timings show the orbital period ischanging. We conclude that spots are very active on thissolar type dwarf and that it may mimic its larger cousins,the RS CVn binaries.Author(s): Robert Hill (Bob Jones University ), Samuel Koenke (BobJones University ), Ronald Samec (Bob Jones University ), Danny Faulkner(University of South Carolina, Lancaster), Walter Van Hamme (FloridaInternational University)

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219.11 – BVRcIc Light Curve Analysis of theShallow Contact Extreme Mass Ratio W UMaBinary, HR BooHR Boo [? (2000) = 14h 48m 33.015s, ? (2000) = +21° 44?01.09"] is an NSVS variable first observed in 1999 andlisted in the 79th name list (Kazarovets, 2008). It wasidentified as a W UMa variable and first characterized bythe period 0.27289 d. This was later corrected to 0.31587d. Various observers have reported ~20 timings ofminimum light over the past ~4000 orbital epochs. Our2012 curve is of high precision, with probable errorsaveraging 5 mmag. The curves have shallow amplitudes,averaging 0.4 magnitudes, yet apparently exhibit totaleclipses. J-K observations yield a G6V type for the system.A linear period determination of 0.31596785(7) d wascomputed with the available timings of minimum light.When the NSVS light curve is considered in the periodstudy, it indicates that the period has been clearlydecreasing over the past 15,000 orbits. The quadratic termfrom this period study is statistically significant at 5 ?. Thisindicates that the binary is evidently undergoing magneticbreaking due to enhanced magnetic solar activity.The lightcurve solution reveals that HR Boo is a shallow contactsystem with a Roche-lobe fill-out of ~4% and a mass ratioof q= 0.25. This is exceedingly rare, since extreme massratio binaries usually have high fill-outs. In addition, anunusually dark 13 degree radius cool spot with a T-factor of~50% was computed near the L1 Point of the primarycomponent. A 32 minute duration of constant light is seenin the secondary eclipse indicating the occurrence of a totaleclipse. This was confirmed in the light curve solution.Although the secondary component has a slightly highertemperature than the primary component, some 30 K, thelight curves have the appearance of an A-type W UMasystem. The system may have come into contact recently.Author(s): Danny Faulkner (Johnson Observatory), Ronald Samec(Astronomy Program, Dept. of Physics and Engineering, Bob JonesUniversity), Travis Shebs (Astronomy Program, Dept. of Physics andEngineering, Bob Jones University), Barry Benkendorf (Astronomy Program,Dept. of Physics and Engineering, Bob Jones University)

219.12 – Simulating Contact BinariesAbout one in every 150 stars is a contact binary system ofWUMa type and it was thought for a long time that such abinary would naturally proceed towards merger, forming asingle star. In September 2008 such a merger was observedin the eruption of a “red nova", V1309 Sco. We aredeveloping a hydrodynamics simulation for contact binariesusing Self Consistent Field (SCF) techniques, so that theirformation, structural, and merger properties could bestudied. This model can also be used to probe the stabilitycriteria such as the large-scale equatorial circulations andthe minimum mass ratio. We also plan to generate lightcurves from the simulation data in order to compare withthe observed case of V1309 Sco. A comparison betweenobservations and simulations will help us better understandthe nova-like phenomena of stellar mergers.Author(s): Kundan Kadam (Louisiana State University), GeoffreyClayton (Louisiana State University), Juhan Frank (Louisiana StateUniversity), Joel Tohline (Louisiana State University), Jan Staff (MacquarieUniversity), Patrick Motl (Indiana University), Dominic Marcello (LouisianaState University)

219.13 – The Interplanetary Medium andAstrosphere around ? Cen A and ? Cen BThe stellar winds of ? Centauri A (HD 128620: G2 V) and B(HD 128621: K1 V) combine to carve a bubble, theastrosphere, into the surrounding interstellar medium. Thewinds and the ISM interact, giving rise to pronouncedastrospheric boundaries including a termination shock andan astropause. Inside the termination shock, the two stellarwinds interact strongly. These interactions have beencharacterized numerically with detailed, time-dependentmodels that also account for the non-equilibrium behaviorof interstellar neutral hydrogen that traverses theastrosphere. The results of this modeling are presented,characterizing the interplanetary environment of extrasolarplanets in the ? Centauri A+B system, and modeledestimates of diffuse, time-dependent X-ray emission due tostellar wind charge exchange are given.Author(s): Hans Mueller (Dartmouth College), Mackenzie Carlson(Dartmouth College)

219.14 – Single Season BVRI Light Curves ofKU Cygni and the Current State of itsEccentric and Variable Accretion DiskKU Cygni is a long period (P=38.4 days) eclipsing Algol-typebinary star. The 0.48 Solar mass K5III secondary componentis presumably undergoing Roche lobe overflow anddonating mass to the 3.85 Solar mass F-type primary. Theresulting accretion disk is large, thick, variable, and verylikely non-circular. A recent study by the Digital Access to aSky Century at Harvard (DASCH) project discovered a ~5year dust accretion event that occurred around 1899 -1904. KU Cyg has also undergone other significant secularvariations that are due to the variability of its accretiondisk. Here, we present a complete single-season multicolorphotometric study of KU Cyg. During our eight monthobserving season in 2013, KU Cyg underwent just sixcomplete orbital cycles. This fact significantly reduces thecomplications of secular variations and therefore theseobservations show us the photometric effects of the currentstate of the circumstellar material. Our analysis of theasymmetries in the primary and secondary eclipses lendsinsight about the current geometry and eccentric nature ofthe accretion disk.Author(s): Phillip Reed (Kutztown University), Katelyn Ciccozzi(Kutztown University)

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219.15 – Investigating mass transfer insymbiotic systems with hydrodynamicsimulationsWe investigate gravitationally focused wind accretion inbinary systems consisting of an evolved star with a gaseousenvelope and a compact accreting companion. We studythe mass accretion and formation of an accretion diskaround the secondary caused by the strong wind from theprimary late-type component using global 2D and 3Dhydrodynamic numerical simulations. In particular, thedependence on the mass accretion rate on the mass lossrate, wind temperature and orbital parameters of thesystem is considered. For a typical slow and massive windfrom an evolved star the mass transfer through a focusedwind results in rapid infall onto the secondary. A streamflow is created between the stars with accretion rates of a2-10% percent of the mass loss from the primary. Thismechanism could be an important method for explainingperiodic modulations in the accretion rates for a broadrange of interacting binary systems and fueling of a largepopulation of X-ray binary systems. We test the plausibilityof these accretion flows indicated by the simulations bycomparing with observations of the symbiotic CH Cygvariable system.Author(s): Miguel de Val-Borro (Princeton Unversity), MargaritaKarovska (Harvard-Smithsonian Center for Astrophysics), Dimitar Sasselov(Harvard-Smithsonian Center for Astrophysics)

219.16 – Constraining the Mass-RadiusRelationship in White Dwarfs UsingGravitational RedshiftsWe present gravitational redshifts (GRs) and masses forover 20 white dwarfs that have distant, non-interactingmain-sequence companions. These are the first results fromour ongoing NOAO programs at the KPNO 4-m and SOAR4.1-m telescopes. We have obtained R~10,000 spectraover three or more epochs for each WD+MS binary andmeasured precise radial velocities and, thus, gravitationalredshifts using the template-matching technique. Thisremoves the subjectivity involved in previous GR studies.Our sample is already the largest set of GRs measured in asingle study, thus, eliminating the systematic differencesbetween different studies and telescopes. We haveobtained independent radius constraints from extantparallax measurements and surface gravity determinationsfrom Balmer series fits to our spectra. By combining ourprecise GR measurements with those values, we obtainedimproved estimates of WD masses and radii. While the WDmass-radius relation underlies much of stellar and galacticastrophysics, only one empirical measurement matches thepredicted value within 3%. Furthermore, the currentpublished sample covers a small range of WD masses. Ourprogram provides more precise measurements of GRs for alarger range of WD mass, spanning 0.5-1.2 Msun.Author(s): Saurav Dhital (Embry-Riddle Aeronautical University),Terry Oswalt (Embry-Riddle Aeronautical University), Jay Holberg(University of Arizona), Trisha Mizusawa (Florida Institute of Technology),Jingkun Zhao (National Astronomical Observatories)

219.17 – A Simple Method to Improve theQuality of RXTE PCA SpectraWe fitted at once all of the several hundred RXTE PCAspectra of the Crab to a simple power-law model; the totalnumber of counts in the composite spectrum is >10^9. Wethen used the spectrum of fit residuals (data/model) tocorrect large samples of spectra of GX~339-4, H1743-322,and XTE J1550-564. The correction improved the quality ofall the fits, and the improvement was dramatic for spectrawith >10^7 counts. The Crab residual spectrum issomewhat different for each of the five PCA detectors, butit was relatively stable during the course of the 16-yearmission. We provide public software that automates theprocess of applying the correction to PCA data andrecommend that the correction be applied to all spectrawith >10^6 counts.Author(s): Javier Garcia (Harvard-Smithsonian Center forAstrophysics), Jeffrey McClintock (Harvard-Smithsonian Center forAstrophysics), James Steiner (Harvard-Smithsonian Center forAstrophysics), Ronald Remillard (Massachusetts Institute of Technology),Victoria Grinberg (Massachusetts Institute of Technology)

219.18 – A Glimpse of Optically VariableGalactic Bulge X-ray Sources: A Comparisonof Mosaic-II and DECam PhotometryWe present optical photometry and spectroscopy ofselected sources from the Galactic Bulge Survey (GBS)using the new DECam imager and the previous Mosaic-IIimager on the 4m Blanco telescope at Cerro-Tololo Inter-American Observatory (CTIO). The goal of the GBS is todetect quiescent Low-Mass X-Ray Binaries (LMXB) andidentify eclipsing systems for follow-up mass determinationto test binary population models and to better determineblack hole and neutron star mass distributions. We comparethe light curves of spectroscopically intriguing sources withboth instruments and show that the DECam observationsdemonstrate large improvements in sensitivity to short-period binary systems. Because of DECam's field of view of2.2 degrees, our survey area can be covered in 4 pointingsas opposed to 64 with Mosaic-II. This increased oursampling rate from 2-5 times to 28-56 times per target pernight, which includes dithering. We find that combining 2x1secs and 2x90 secs exposures over a two day observingrun, we can detect targets between 12th and 23rdmagnitude. Overall, we are finding that DECam is a superbinstrument for detecting variability of sources in wide-fieldoptical surveys. This work was supported by the NationalScience Foundation under Grant No. AST-0908789 and byNASA through Chandra Award Number AR3-14002X issuedby the Chandra X-ray Observatory Center, which isoperated by the Smithsonian Astrophysical Observatory forand on behalf of the National Aeronautics SpaceAdministration under contract NAS8-03060.Author(s): Christopher Johnson (Louisiana State University), RobertHynes (Louisiana State University), Peter Jonker (Harvard-SmithsonianCenter for Astrophysics), Manuel Torres (Harvard-Smithsonian Center forAstrophysics), Chris Britt (Texas Tech. University), Danny Steeghs(University of Warwick), Tom Maccarone (Texas Tech. University), GijsNelemans (IMAPP, Radbound University), Sandra Greiss (University ofWarwick), Austin Baldwin (Louisiana State University)

Contributing teams: The Galactic Bulge SurveyCollaboration

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219.19 – Searching for a Spin-SuperorbitalPeriod-Relation in Bright X-ray BinariesThanks to long-term X-ray monitoring, a number of closeX-ray binaries are now known to show X-ray periodicities ontimescales of at least tens of binary orbital timescales, forwhich the current favorite model is warping and precessionof the accretion disk. In at least one case, the period of thissuperorbital variation is known to change relativelysmoothly on a timescale of years. Initial indications fromarchival data suggest that the neutron star's pulse periodmay also vary on a similar timescale from the same object.If confirmed, this would observationally demonstrate adirect link between the properties of the accretion diskprecession and the mass transfer rate onto the neutron staraccretor. We have undertaken a campaign to systematicallysearch for just such a link, using archival RXTE data goingback to 1996. This poster describes our techniques andscience results.Author(s): Kristen Dage (University of Michigan-Dearborn), WilliamClarkson (University of Michigan-Dearborn)

219.20 – The Orbital Light Curve of theLow-Mass X-ray Binary V1408 AquilaeWe have obtained high-speed optical photometry of the lowmass X-ray binary V1408 Aquilae (= 4U 1957+115),totaling 126 hours of data obtained on 29 nights. Theorbital light curve of the system has a large-amplitude androughly-sinusoidal modulation. We fit the data withsynthetic light curves calculated from a model thatincludes: (1) a black hole primary surrounded by (2) anaxisymmetric, optically-thick, physically-thin, viscous,steady-state accretion disk, that is fed from (3) a low-mass,cool secondary star. The secondary star is strongly heatedby radiation from the disk. The varying aspect of thesecondary's heated face dominates the orbital light curveand is the source of the quasi-sinusoidal modulation. Wepresent the results of an extensive exploration of themodel's parameter space.Author(s): Sebastian Gomez (University of Texas-El Paso), PaulMason (University of Texas-El Paso), Edward Robinson (University of Texas)

219.21 – Polarization of the Cygnus X-1SystemWith broadband optical polarimetry, we have observed theCygnus X-1 system using the POLISH2 polarimeter at theLick Observatory 1-m telescope. We have observed thissystem for a total of 19 nights during July, August, andSeptember of 2012, and June of 2013, with the goal ofconstraining orbital inclination and determining the truemass of the black hole in the system. While Kemp et al.made a significant effort to determine this mass in the1980’s, it was unsuccessful due to limitations in instrumentsensitivity and the complexities of the rapidly evolvingsystem. We aim to improve upon this effort with our data,which achieves 0.01% sensitivity simultaneously in the Bband for both linear and circular polarization. Furtherobservations in UBV bands are planned for the spring andsummer of 2014 in order to study the black hole andsupergiant system continually, as it evolves throughout its5.6-day orbital period. We present results of our initial, highSNR observations that show dramatic changes inpolarization of signal taken one month apart. We also findthat the circular polarization (Stokes V) appears morephase-locked than the linear polarization (Stokes Q and U),indicating a strong possibility that we are observing the jetof the black hole. This work is supported by UCO/LickObservatory.Author(s): Larissa Nofi (University of California, Santa Cruz),Sloane Wiktorowicz (University of California, Santa Cruz)

219.22 – Soft X-ray Excesses and X-ray LineVariability in Cygnus X-3Cygnus X-3 is an X-ray binary (XRB) system containing astellar-mass compact object, most likely a black hole, and aWolf-Rayet companion star, which produces collimated,relativistic jets, placing it in the sub-class of XRBs known asmicroquasars. During a Swift/XRT monitoring program ofCygnus X-3, a soft X-ray excess (below 1 keV) was observedat certain states and phases of activity. This soft excessappears to be similar to the variable soft emission observedin Seyfert galaxies. The presence of these features inCygnus X-3 would argue for a greater support of theblack-hole nature of the compact object and serve to betterhighlight the similarities of microquasars and AGN. Wepresent the results of our investigations of these softexcesses, as well as the variations of the X-ray Fe lineregion (6.4-7.0 keV) as a function of the state activity andorbital phase.Author(s): Angelo Varlotta (SAO), Michael McCollough (SAO)

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219.23 – Faraday Structure of the Jets of theMicroquasar SS433. I. Rotation MeasureDistributionWe report a detailed study of the Faraday rotation in thejets of SS433 using five epochs of data from the Jansky VLA.Observations spanning 4.5-8.5 GHz were used to createlinear polarization images in multiple spectral windowsusing CASA, and the data passed to AIPS for analysis. Weused both the traditional rotation measure derivation taskRM and the Faraday rotation measure synthesis task FARSto derive the distribution of the Faraday rotation measure("RM") across the source. We find it to be non-uniform,indicating that at least part of the RM is local to the source.We track the evolution of the RM structure over a period ofabout 50 days and find significant changes, furthersupporting the local origin of some of the rotation. In acompanion paper we attempt to correlate the RM structurewith the well-known 3-D morphology of the jets.Author(s): Michael Kosowsky (Brandeis University), David Roberts(Brandeis University), John Wardle (Brandeis University)

219.24 – Faraday Structure of the Jets of theMicroquasar SS433. II. Modeling the Sourcein 3-DIn a companion paper we report Jansky VLA observations ofthe Faraday rotation measure structure of the jets in SS433.Here we analyze those data in light of the well-known 3-Dstructure of the source using Faraday rotation measuresynthesis ("FRMS"). The power of FRMS is that in principle itpermits us to determine the 3-D structure of thesynchrotron emissivity and of the product of thelongitudinal component of the magnetic field and thethermal particle distribution. We combine the Faradaydepth structure of SS433 revealed in our FRMS analysiswith information from the linear polarization of theobserved synchrotron emission and the known 3-D sourcemorphology. From this we attempt to build a model of themagnetic field in three dimensions that is consistent withall of the data.Author(s): David Roberts (Brandeis Univ.), Michael Kosowsky(Brandeis Univ.), John Wardle (Brandeis Univ.)

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220 – Molecular Clouds and Dust PostersPoster Session – Essex Ballroom and America Foyer – 03 Jun 2014 09:00 AM to 06:30 PM

220.01 – Enigmatic Extinction: AnInvestigation of the 2175Å Extinction Bumpin M101Evidence from studies of starburst galaxies indicates thatactive formation of high mass stars modifies the UV dustextinction curve as seen by a lack of the characteristic2175Å bump. For over 45 years, the source of the 2175Åextinction feature has yet to be positively identified. Smallaromatic/PAH grains are suggested as a leading contenderin dust grain models. The face-on spiral galaxy M101 is anideal laboratory for the study of dust, with manywell-studied HII regions and a steep metallicity andionization gradient. The Interstellar Medium AbsorptionGradient Experiment Rocket (IMAGER) probes thecorrelation between dust extinction, and the metallicity andradiation environment in M101 at ultraviolet wavelengths.IMAGER simultaneously images M101 in three 400Å-widebandpasses, measuring the apparent strength of the 2175Åbump and the UV continuum. Combining data from IMAGERwith high S/N far- and near- UV observations from theMAMA detectors on the Hubble STIS instrument, weexamine the apparent strength of the 2175Å bump in HIIregions of M101. With additional infrared data from Spitzer,the DIRTY radiative transfer model, and stellar evolutionmodels, we probe the correlation between the 2175Åfeature and the aromatic/PAH features across HII regions ofvarying metallicity and radiation field hardness. The resultsof this experiment will directly impact our understanding ofthe nature of dust and our ability to accurately account forthe effects of dust on observations at all redshifts.Author(s): Meredith Danowski (Massachusetts Institute ofTechnology), Timothy Cook (University of Massachusetts- Lowell), KarlGordon (Space Telescope Science Institute), Supriya Chakrabarti(University of Massachusetts- Lowell), Brandon Lawton (Space TelescopeScience Institute), Karl Misselt (University of Arizona)

220.02 – COS/HST Local Interstellar MediumAnalysis and Kinematic Survey using WhiteDwarfs (CLIMAKS)Objects with well-constrained continua are extremelywell-suited to studies of the interstellar medium; whitedwarfs are of particular use in this regard. We present herefurther analysis of archival HST-Cosmic OriginsSpectrograph spectra of 36 white dwarfs within 100 pc.These spectra are part of a much larger sample, obtainedas part of a large scale survey by Gaensicke et al. todetermine the extent of pollution from circumstellar debrisdisk reaccretion. The sensitivity of the COS instrument andthe quality of the WD models combine to make this dataset very suitable for studying the properties of the localISM. We have analyzed and fit the spectra to determine thecharacteristics of the intervening ISM absorber(s),specifically in CII/CII*, NI, OI, and SiII/SiII*/SiIII. From theresults of such analyses, we can extract values for thekinematics, abundances, electron density, ionizationstructure, and physical size of the absorbing cloud(s). Giventhe sample size, it is also possible to use thesemeasurements to refine preexisting kinematic models ofthe various LISM absorbing clouds.Author(s): Benjamin Tweed (Wesleyan University), Seth Redfield(Wesleyan University), Boris Gaensicke (University of Warwick), DetlevKoester (University of Kiel), Jay Farihi (University College London)

220.03 – A Direct Measurement of theCO/H2 Abundance Ratio in the MagellanicCloudsTheoretical and observational evidence suggests thatmolecular gas (H2) is not always correlated with COemission, because CO is photo-dissociated more easily thanH2. The mass of CO-poor H2 present in the envelopes ofgiant molecular clouds (GMCs) is expected to be higher inlow metallicity GMCs, which are more exposed todissociating radiation due to their lower dust abundance.Since we cannot detect H2 directly, the mass of theseCO-poor envelopes is effectively "hidden" from radiotelescopes. As a result, theoretical predictions of the CO/H2abundance, are difficult to test and validate, and theamount of molecular gas present in low metallicity galaxiesis not well constrained. The most sensitive andunambiguous way to determine CO and H2 columndensities is to derive them from UV absorptionspectroscopy. We have acquired high S/N spectra of the 4thpositive absorption band of CO with HST/COS toward 9translucent (AV~1) Magellanic Cloud sight-lines probing theedges of GMCs, for which previous FUSE spectra and H2column density determinations are available from the FUSEcatalogs and archive. After removing spectral featuresassociated with the stellar sources, we find CO columndensities as low as ~1013 cm-2 toward those translucentsight-lines. We have computed the CO and H2 abundancesas a function of total gas column and extinction, and havefound this relation to be compatible with predictions fromnumerical models of CO and H2 formation and dissociation.The cooling rate associated with CO rotational emissionappears to be negligible compared to cooling by ionizedcarbon (C II) in this density regime.Author(s): Julia Roman-Duval (Space Telescope Science Institute),Mark Krumholz (University of California at Santa Cruz), Alberto Bolatto(University of Maryland), Karl Gordon (Space Telescope Science Institute),Christopher McKee (University of California at Berkeley), Jason Tumlinson(Space Telescope Science Institute)

220.04 – C15N in Diffuse Molecular CloudsWe report the first detection of C15N in absorption in diffusemolecular gas from a detailed examination of archivalVLT/UVES data covering the CN lines near 3875 Å.

Absorption from the C15N isotopologue is detected in threeout of the four directions studied and appears as a very

weak feature between the main 12CN and 13CN absorptionlines. Column densities for each CN isotopologue aredetermined through profile fitting, after accounting forweak additional line-of-sight components, which are

observed in CH and CH+. The weighted mean value of

C14N/C15N for the three sight lines with detections of C15Nis 277±16, in very good agreement with the terrestrial14N/15N ratio of 272. Our results help to clarify the situationregarding the nitrogen isotope ratio in the solarneighborhood, with important implications for interstellarchemistry and Galactic chemical evolution.Author(s): Steven Federman (Univ. of Toledo), Adam Ritchey (Univ. ofWashington), David Lambert (McDonald Observatory)

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220.05 – A 3D Dust Map from PanSTARRS 1We present a 3D map of dust reddening in the Milky Way,using photometry from more than half a billion wellobserved stars in the PanSTARRS 1 (PS1) 3pi survey. Wegroup stars into pixels, and then infer the line-of-sightreddening vs. distance relation from the individual stellarreddenings and distances. We derive the full probabilitydensity of reddening as a function of distance in each~7'x7' pixel on the sky, incorporating prior knowledgeabout the distribution of stars throughout the Galaxy and5-band PS1 photometry. We show that in the large-distancelimit, our 3D map has good agreement with theemission-based 2D dust map of Schlegel, Finkbeiner &Davis (1998), despite the very different datasets andmethods the two maps rely on. A greater understanding ofthe 3D distribution of dust in the Galaxy will allow a wealthof detailed science in the Galactic plane, where dusthinders stellar parameter estimation and obscuresstructure. The method we use can be extended to takeadvantage of other datasets, such as 2MASS, WISE, SDSSand, eventually, LSST.Author(s): Gregory Green (Harvard Univ.), Eddie Schlafly (MPIA),Douglas Finkbeiner (Harvard Univ.)

220.06 – The Galactic Plane InfraredPolarization Survey (GPIPS): FinalCalibration and Full Data ReleaseAll observations for the Galactic Plane Infrared PolarizationSurvey (GPIPS) have been completed on the 1.8m Perkinstelescope with the Mimir near-infrared instrument. Finalcalibration has been established and applied, andpolarization and photometric data products (catalogs andimages) have been released for general use. GPIPSsurveyed 76 sq deg of the northern Galactic plane, from L= 18 to 56 deg and B = -1 to +1 deg, in the H-band (1.6?m). The survey was conducted over 360 telescope nightsbetween 2006 and 2013 as 3,237 dithered sky placementsof the 10x10 arcmin FOV of Mimir. Pixel sampling of 0.58arcsec was well-matched to the average seeing of 1.5arcsec; all GPIPS data met a 2 arcsec seeing criterion. Thecalibration process utilized stars in globular cluster fields,mostly off the Galactic plane along low extinctionsightlines, and in specific fields hosting multiplepolarization standard stars. The polarization calibrationfloor is under 0.1% for single observations. GPIPS sampledstellar polarizations from 7th to 12th mag in H-band,resulting in nearly 1 million stars with measuredpolarizations, which probed directions with up to 20-30 magof visual extinction. GPIPS data are ideal for mapping plane-of-sky magnetic field orientations in interstellar gas anddust clouds, identifying regions of star formation, anddiscovering stars with circumstellar scattering duststructures. Tools for accessing and exploring the GPIPS dataproducts have been developed and will be highlighted.GPIPS has been supported through NSF grants AST06-07500 and 09-07790.Author(s): Dan Clemens (Boston University), Lauren Cashman(Boston University), Sadia Hoq (Boston University), Jordan Montgomery(Boston University), Michael Pavel (Boston University)

220.07 – Testing for Helical Magnetic Fieldsin the Orion Molecular Cloud Integral-Shaped FilamentThe Orion Molecular Cloud (OMC) is one of the closest andmost well-studied regions of ongoing star formation. Withinthe OMC, the Integral-Shaped Filament (ISF) is a long,filamentary structure of gas and dust that stretches over 7pc and is itself comprised of many smaller filaments. Radialdensity profiles of the ISF indicate that these filamentarystructures may be supported by helical magnetic fields(Johnstone & Bally 1999). To test for the presence of helicalfields, we have collected deep near-infrared (NIR) H-band(1.6 ?m) and K-band (2.2 ?m) linear polarimetry ofbackground starlight for a grid of six 10x10 arcmin fields ofview fully spanning the ISF. NIR polarizations from scatteredlight and young stellar objects, which do not trace themagnetic field, are identified by examining the ratio ofpercent polarization in H-band to K-band. The data werecollected using the Mimir NIR instrument on the 1.8mPerkins Telescope located outside of Flagstaff, AZ. This workis partially supported by NSF grant AST 09-07790.Author(s): Lauren Cashman (Boston Univ.), Dan Clemens (BostonUniv.)

220.08 – High-Mass Star Formation inIRDCs: The Role of Magnetic FieldsThe role of the Galactic magnetic field in creatinghigh-mass stars within Infrared Dark Clouds (IRDCs) is notwell understood. Three prevailing theories describing thenature of the magnetic field are strong-field models,weak-field models, and helical fields. Each has differentimplications of how the field affects cloud and starformation. We use a sample of 30 IRDCs in the first Galacticquadrant to study the relationships between magneticfields and cloud properties. To trace the magnetic field inthe vicinity of the clouds, we use near-infrared (NIR) H (1.6?m) and K-band (2.2 ?m) polarimetric observations ofbackground starlight from the Mimir instrument on the1.8m Perkins telescope. The Herschel Hi-GAL Survey of dustcontinuum emission was used to estimate the IRDC columndensities, and the Spitzer GLIMPSE & MIPSGAL Surveyswere used to find their level of star formation activity. Wedetermine whether the direction of the magnetic fieldinferred from the NIR polarizations differentiate betweenthe different magnetic field models, and whether anycorrelations exist between magnetic field properties(direction and dispersion) and IRDC properties, such asdensity and level of star formation activity. This work ispartially supported by NSF grant AST 09-07790.Author(s): Sadia Hoq (Boston Univ.), Dan Clemens (Boston Univ.)

220.09 – Spitzer observations of infraredcirrus around embedded B starsI discuss IRAC and MIPS observations of the infrared cirrusaround two embedded B stars, HR 5336 and HR 890. IRASobservations have previously shown a deficit in mid-IRemission relative to longer infrared wavelengths for the ISMaround these objects. The deficit suggests that small dustgrains (VSGs and PAHs) are depleted in the vicinity of theUV radiation field from these stars. Color maps from 3-160microns are presented and the relative abundances of eachgrain population are modeled using DUSTEM.Author(s): Sean Carey (Caltech)

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220.10 – Bow-Shock Nebulae in the WISEAll-Sky Survey: Around the CelestialEquatorThis is a preliminary survey for bow-shock nebulae withinone degree of the celestial equator using the WISE All-SkyData Release. Bow-shock nebulae are clumps of gas anddust that have been condensed by the winds of starsmoving through the interstellar medium. This survey hasdiscovered twenty-four bow-shock nebula candidates andtheir candidate wind-blowing stars. bow-shocks werepreferentially found at low galactic latitudes and near theGalactic Center and Anti-Center, as expected. Intriguinglyand contrary to previous assumptions, they were not foundprimarily around OB-runaway stars. A third of thebow-shock nebulae we discovered were around T Tauri starsor young stellar objects (YSOs). Even more unexpectedly,another third of the bow-shock nebulae we found arearound A- and F-type stars, which seem too cool to excitethe nebulae. This research was funded by a NASA Californiaspace grant.Author(s): Kendall Hall (California State Univ., Fresno), FredRingwald (California State Univ., Fresno)

220.11 – The hydration dependence ofCaCO3 absorption lines in the Far IRThe far infrared (FIR) absorption lines of CaCO3<\sub>have been measured at a range of relative humidities (RH)between 33 and 92% RH using a Bruker 66v/Sspectrometer. Hydration measurements on CaCO3<\sub>have been made in the mid-infrared (MIR) by [Al-Hosney,H.A. and Grassian, V.H., 2005, Phys. Chem. Chem. Phys., 7,1266], and astrophysically-motivated temperature-dependent FIR measurements of CaCO3<\sub> in vacuumhave also been reported [Posch, T., et al., 2007, Ap. J., 668,993]. The custom sample cell constructed for thesehydrated-FIR spectra is required because the 66v/S benchis under vacuum (3 mbar) during typical measurements.Briefly, the sample cell consists of two ThaliumBromoiodide (KRS-5) windows, four O-rings, a plastic ringfor separating the windows and providing a volume for thesaturated atmosphere. CaCO3<\sub> was deposited onKRS-5 windows using doubly-distilled water as anintermediary. The KRS-5 window with sample andassembled sample cell were placed in a desiccator with theappropriated saturated salt solution [Washburn, E.W. (Ed.),International Critical Tables of Numerical Data, PhysicsChemistry and Technology, Vol. 1, (McGraw-Hill, New York,1926), p. 67-68] and allowed to hydrate for 23 hours. Forspectroscopy the desiccator was quickly opened and thesecond KRS-5 window placed in the cell to seal thechamber. A spectrum was then taken of the sample at theappropriate RH. The spectra taken characterize theadsorption of water vapor and CaCO3<\sub> that mightoccur in circumstellar environments [Melnick, G.J., et al.2001, Nature, 412, 160]. The MIR and FIR reflectancespectra of calcite (CaCO3<\sub>) have been thoroughlystudied by [Hellwege, K.H., et al., 1970, Z. Physik, 232, 61].Five Lorentzian curves were fit to our data in the rangefrom 378-222 cm-1<\sup> and each was able to beassigned to a known mode of CaCO3<\sub>. The data doesnot support the conclusion of a hydration effect on thesemodes of CaCO3<\sub>, but it does suggest a possiblebroadening of three modes peaked at 281 cm-1<\sup>.The goal of this work is to bridge the body of work onCaCO3<\sub> in physical chemistry and previouslaboratory astrophysical observations to aid interpretationof FIR spectra obtained by observatories such as theSpitzer Space Telescope.Author(s): Johnny Powell (Reed College), Logan Emery (Reed College)

220.12 – A Herschel-SPIRE Survey of theMonR2 Giant Molecular CloudWe present a new survey of the MonR2 giant molecularcloud with SPIRE on the Herschel Space Observatory. Wecross-calibrated SPIRE data with Planck-HFI and accountedfor its absolute offset and zero point correction. We fixedemissivity with the help of flux-error and flux ratio plots. Asthe best representation of cold dusty molecular clouds, wedid greybody fits of the SEDs. We studied the nature ofdistribution of column densities above and below certaincritical limit, followed by the mass and temperaturedistributions for different regions. We isolated the filamentsand studied radial column density profile in this cloud.Author(s): Riwaj Pokhrel (University of Massachusetts), RobertGutermuth (University of Massachusetts), Babar Ali (IPAC, Caltech), S.Thomas Megeath (U of Toledo), Judith Pipher (U of Rochester), Philip Myers(Harvard University), William Fischer (U of Toledo), Thomas Henning (MaxPlanck Institute for Astronomy), Scott Wolk (Harvard University), Lori Allen(NOAO), John Tobin (NRAO)

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220.13 – A New Method of FIR Modeling ofFilamentary IRDCsWe present a novel method to extract high spatialresolution dust column density and temperature mapsassociated with filamentary infrared dark clouds (IRDCs).We combine the usual cloud far-infrared emission fromSPIRE bands with the higher resolution absorption imagesat the PACS bands. Our approach allows us to obtain moreprecise temperatures and column density maps at the bestangular resolution available in the data, set by the PACS70micron beam size, but it requires careful modeling of theGalactic background and foreground emission. The methodis especially useful to study the remarkable sample ofIRDCs unveiled by Herschel, which are cold and denseenough to appear in absorption against the Galacticfar-infrared background at 70 ?m. For these IRDCs, wecompare our method with physical parametersindependently derived from continuum and molecular linedata, and find consistent results.Author(s): Andres Guzman (Harvard Smithsonian Center forAstrophysics), Howard Smith (Harvard Smithsonian Center forAstrophysics), Juan Rafael Martinez-Galarza (Harvard Smithsonian Centerfor Astrophysics)

220.14 – Two-component Thermal DustEmission Model: Application to the PlanckHFI MapsWe present full-sky, 6.1 arcminute resolution maps of dustoptical depth and temperature derived by fitting theFinkbeiner et al. (1999) two-component dust emissionmodel to the Planck HFI and IRAS 100 micron maps. Thisparametrization of the far infrared thermal dust SED as thesum of two modified blackbodies serves as an importantalternative to the commonly adopted single modifiedblackbody dust emission model. We expect ourPlanck-based maps of dust temperature and optical depthto form the basis for a next-generation, high-resolutionextinction map which will additionally incorporatesmall-scale detail from WISE imaging.Author(s): Aaron Meisner (Harvard University), Douglas Finkbeiner(Harvard University)

220.15 – Towards a Unified Model ofPolarized Emission and Extinction fromInterstellar DustWe present models of interstellar grains that reproduceobservational constraints on dust extinction, polarizedextinction, infrared emission, and elemental abundances.Employing spheroidal graphite-PAH and "astrosilicate"grains of varying axial ratio, we constrain the sizedistribution and degree of alignment as a function of grainsize. We discuss in particular the polarized emission fromeach model in the context of results from Planck as well asthe effects of including contributions from ferromagneticiron nanoparticles. We outline our next steps in developinga model of dust in the diffuse ISM by leveragingobservational constraints on scattering and adapting ourmodels to environments other than the diffuse ISM.Author(s): Brandon Hensley (Princeton University), Bruce Draine(Princeton University)

220.16 – Grain Destruction in EvolvingSupernova RemnantsSupernova remnant (SNR) shocks are believed to be theprimary regions of destruction for interstellar dust grains.This destruction occurs primarily because of the grainacceleration that occurs when the shock causes the gasand magnetic field to be compressed. Most calculations ofgrain destruction in shocks have used steady, plane parallelshocks, but in the interstellar medium most shocks resultfrom SNRs and have significant time dependent andnon-planar effects. We present new results for graindestruction that use numerical hydrodynamical calculationsof supernova remnant evolution and include all importantgrain processes. We show that the lower density behindSNR shocks leads to substantially less grain destruction,alleviating the discrepancy between the grain destructionand creation timescales for silicate grains.Author(s): Jonathan Slavin (Harvard-Smithsonian, CfA)

220.17 – Collision of High Velocity Cloudswith the Galactic Disk under the Effect ofDark MatterThe fate of high velocity clouds (HVCs) will affect theevolution of the Milky Way. If currently observed HVCssurvived the interaction with the halo gas and reached theGalactic disk eventually, HVCs could provide fuel for thestar formation in the disk. For this reason, the collision ofHVCs with the Galactic disk has been extensively studiedvia numerical simulations. Recently, an idea that someHVCs are accompanied by dark matter has been suggestedbased upon the scenario that HVCs originated from thestripped gas of satellite galaxies which tend to have darkmatter. Along the similar line of reasoning, it is worthinvestigating the effect of dark matter on the collision ofHVCs with the Galactic disk. By using the FLASHhydrodynamics code, we simulate this scenario and searchfor proper parameters of dark matter and baryonic matterthat can explain the currently available observations suchas the Smith Cloud.Author(s): Kyujin Kwak (Ulsan National Institute of Science andTechnology (UNIST)), Hyun Taek Lee (Ulsan National Institute of Scienceand Technology (UNIST)), Seungwon Yang (Ulsan National Institute ofScience and Technology (UNIST)), Kwang Hyun Sung (Ulsan NationalInstitute of Science and Technology (UNIST)), Jongsoo Kim (KoreaAstronomy and Space Science Institute (KASI))

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221 – AGN, QSO, Blazars PostersPoster Session – Essex Ballroom and America Foyer – 03 Jun 2014 09:00 AM to 06:30 PM

221.01 – The Clustering of Quasars atRedshift 2.5 from the Final SDSS-III/BOSSSampleMeasuring the mass of the dark matter halos that hostquasars is a critical question in the field of galaxy evolution.Estimates of how the mean mass of the dark matter halosin which quasars are triggered evolves with time canpotentially constrain scenarios in which the quasar phase istriggered in different dark-matter environments as theUniverse progresses. Quasar clustering measurements onlinear scales across a range of redshifts is a powerful toolwith which to estimate the masses of the dark matter halosthat are inhabited by the galaxies that host quasars.Although there are many measurements of quasarclustering at redshift z < 2.2, and a few at z > 3, there arevery few precise measurements around z~2.5, where thequasar phase appears to peak before declining at z < 2.The SDSS-III/BOSS survey targets redshifts of 2.2 < z < 3.5,and should therefore offer the most precise estimates ofquasar clustering near the epoch of peak quasar activity.We use data from SDSS-III/BOSS to measure the clusteringof quasars over the redshift range 2.2 < z < 2.8 via the realand redshift space two point correlation functions. The dataconsists of a homogeneously selected sample of 62960BOSS CORE quasars drawn from SDSS DR11. Ourhomogeneous sample covers ~4460 (deg)^2corresponding to a comoving volume of ~12 (Gpc/h)^3. Weobtain the correlation length of quasars near z~2.5 andderive the bias of the dark matter halos that host quasars.We study the mass of the dark matter environments ofquasars using the formalism of the Halo OccupationDistribution (HOD). We will discuss our results at z~2.5, andalso results obtained by dividing the BOSS quasar sampleinto three redshift ranges to study how the correlationlength, bias, and dark matter halo mass of quasars evolveover this key redshift range.Author(s): Sarah Eftekharzadeh (Department of Physics andAstronomy, University of Wyoming), Adam Myers (Department ofPhysics and Astronomy, University of Wyoming), Martin White(Department of Phhysics and Astronomy,University of CaliforniaBerkeley,601 Campbell,94720), Jo Bovy (Institute for Advanced Study,Einstein Drive, Princeton, NJ 08540), Xiaohui Fan (Steward Observatory,The University of Arizona), Jean-Marc Le Goff (CEA, Centre de Saclay,Irfu/SPP, 91191), Pierre Laurent (CEA, Centre de Saclay, Irfu/SPP, 91191),Cameron McBride (Harvard-Smithsonian center for Astronomy,60 GardenStreet,MA 02138), Jordi Miralda-Escude (Institut de Ciencies del Cosmos,Universitat de Barcelona), Nathalie Palanque-Delabrouille (CEA, Centre deSaclay, Irfu/SPP, 91191), Patrick Petitjean (Universit Paris 6 et CNRS,Institut dAstrophysique de Paris, 98bis blvd. Arago, 75014 ), Nicholas P.Ross (Lawrence Berkeley National Laboratory, One Cyclotron Road,Berkeley, CA 94720), Donald Schneider (Dept. Astron. & Astrophys. andInstitute for Gravitation & the Cosmos, Pennsylvania State University,University Park, PA 16802), Yue Shen (Harvard-Smithsonian center forAstronomy,60 Garden Street,MA 02138), Michael Strauss (Department ofAstrophysical Sciences, Princeton University ), Alina Streblyanska (Institutode Astrofisica de Canarias (IAC), E-38200 La Laguna), David Weinberg(Department of Astronomy and CCAPP, Ohio State University), W.Wood-Vasey (Pittsburgh Particle Physics, Astrophysics, and CosmologyCenter (PITT PACC), Physics and Astronomy Department, University ofPittsburgh,PA 15260), Matteo Viel (INAF Osservatorio Astronomico viaTiepolo 11 I-34143 ), Christophe Yeche (CEA, Centre de Saclay, Irfu/SPP,91191), Don York (Department of Astronomy and Astrophysics, Universityof Chicago, 5640 South Ellis Avenue,IL 60637), Idit Zehavi (Department ofAstronomy, Case Western Reserve University)

221.02 – AGN Feedback in the Hot Halo ofNGC 4649Using the deepest available Chandra observations of NGC4649 we find strong evidences of cavities, ripples and ringlike structures in the hot interstellar medium (ISM) thatappear to be morphologically related with the central radioemission. These structures are reminiscent of the structuresobserved in NGC 1275 Chandra images. In common withthat source, we found no significant temperature variationsin correspondence with higher pressure regions (0.5 kpc < r< 3 kpc), suggesting that the observed structures may beisothermal waves whose energy is dissipated by viscosity.On the same spatial scale, a discrepancy between the massprofiles obtained from stellar dynamic and Chandra datarepresents the telltale evidence of a significant non-thermalpressure component in this hot gas, which is related to theradio jet and lobes. On larger scale we find agreementbetween the mass profile obtained form Chandra data andplanetary nebulae and globular cluster dynamics. Thenucleus of NGC 4649 appears to be extremely radiativelyinefficient, with highly sub-Bondi accretion flow.Consistently with this finding, the jet power evaluated fromthe observed X-ray cavities implies that a small fraction ofthe accretion power calculated for the Bondi mass accretionrate emerges as kinetic energy. Comparing the jet power toradio and nuclear X-ray luminosity the observed cavitiesshow similar behavior to those of other giant ellipticalgalaxies.Author(s): Alessandro Paggi (Harvard-Smithsonian Center forAstrophysics), Giuseppina Fabbiano (Harvard-Smithsonian Center forAstrophysics), Dong-Woo Kim (Harvard-Smithsonian Center forAstrophysics), Francesca Civano (Harvard-Smithsonian Center forAstrophysics), Jay Strader (Department of Physics and Astronomy,Michigan State University)

221.03 – Disk Wind Mass Loss Estimates inQSOsWe derive here a relatively simple expression for the totalwind mass loss rates in QSOs within the accretion disk windscenario. We show that the simple expression derived herefor QSO disk wind mass loss rate is in very good agreementwith the more “exact” values obtained through significantlymore complex and detailed numerically intensive 2.5Dtime-dependent simulations. Additionally we show that fortypical QSO parameters, the disk itself will be emittingmostly in the UV/Optical spectrum, in turn implying that theX-ray emission from QSOs likely is produced through somephysical mechanism acting at radii smaller than the innerdisk radius (for a standard accretion disk, half of the initiallygravitational potential energy of the accreting disk mass isemitted directly by the disk, while the other half “falls”closer towards the black hole than the inner disk radius).We also show that for typical QSO parameters, the diskitself is dominated by continuum radiation pressure (ratherthan thermal pressure), resulting in a “flat disk” (except forthe innermost disk regions).Author(s): Nicolas Pereyra (University of Texas - Pan American)

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221.04 – Radio-Loud and Radio-Quiet BALQuasars Differ Only in Their RadioPropertiesRecent studies of the rest-frame ultraviolet(observed-frame optical) spectral properties of radio-loudbroad absorption line (BAL) and radio-loud non-BAL quasarshave shown that they are quite similar. Here we extend thisanalysis to compare spectral properties in radio-loud (73)and radio-quiet (472) BAL quasars selected from the SloanDigital Sky Survey (SDSS). The samples have similarredshift ranges (from 1.5 to 3.5) and broad-bandluminosities. We compare several continuum, emission-line,and absorption-line properties. While most spectralproperties in the two samples have no significantdifferences, we find that the properties of the CIV emissionline may differ slightly. However, CIV is difficult to measurein BAL quasars due to the strong absorption, and we findevidence that the apparent CIV differences may be relatedto small but systematic differences in the velocity structureof the BAL wind in radio-loud compared to radio-quietobjects. We conclude that radio-loud and radio-quiet BALQSOs have few physical differences, except for their radioproperties. This indicates that results using samples ofradio-loud BAL quasars extend to their radio-quietcounterparts, and the two do not form significantly differentsubclasses.Author(s): Thomas Rochais (University of Wyoming), MichaelDiPompeo (University of Wyoming), Adam Myers (University of Wyoming),Michael Brotherton (University of Wyoming)

221.05 – Breaking Degeneracies betweenQuasar Halo Occupation DistributionModels: Extending Direct Measurements ofthe Mean Occupation Distribution toRedshift 0.6Recent work on quasar clustering suggests a degeneracy inthe halo occupation distribution (HOD) constrained fromtwo-point correlation functions. To break this degeneracy,we made the first direct measurement of the meanoccupation function (MOF) of quasars at redshift z ~ 0.2from cross-matching SDSS DR7 quasars with clusters ofgalaxies drawn from the MaxBCG catalog. A limitation ofour measurement is that at z ~ 0.2 the number of quasarsdeclines rapidly compared to at higher redshift. Tocircumvent this limitation, we repeat our measurementusing clusters drawn from the RedMapper catalog. Thenumber of matched quasars increases significantly in thisnew analysis, as RedMapper clusters probe as high as z ~0.6. Preliminary results show that the MOF increasesmonotonically with halo mass. We also measure thevariance, the second moment of the HOD, which closelyresembles a Poisson distribution. The radial distribution ofquasars within dark matter halos is well described by apower law with a slope of ~ -1. The conditional luminosityfunction (CLF) of quasars and conditional black hole massfunction (CMF) show no dependence with host halo mass,similar to inferences drawn from measurements of thetwo-point correlation function.This work is supported by theNational Science Foundation through grant number1211112 and by NASA through ADAP award NNX12AE38G.Author(s): My Nguyen (University of Wyoming), SuchetanaChatterjee (Presidency University), Adam Myers (University of Wyoming),Zheng Zheng (University of Utah), Eduardo Rozo (Stanford University), EliRykoff (Stanford University)

221.06 – Structure Function Analysis of AGNVariability using KeplerWe study the variability properties of AGN light-curvesobserved by the Kepler satellite. AGN optical fluxes areknown to exhibit stochastic variations on time-scales ofhours, days, months and years. Previous efforts tocharacterize the stochastic nature of this variability havebeen hampered by the lack of high-precision space-basedmeasurements of AGN fluxes with regular cadence. Kepler

provides light-curves with a S/N ratio of 10-5 for 87 AGNobserved over a period of ~ 3 years with a cadence of onceevery 30 minutes allowing for a detailed examination of thevariability process. We probe AGN variability using theStructure Functions of the light-curves of the Kepler AGN.Monte-Carlo simulations of the structure function are usedto fit the observed light-curve to models for the PowerSpectral Density. We test various models for the form of thePSD including the damped random walk and the poweredexponential models. We show that on the shortertime-scales probed by Kepler data, the damped randomwalk model fails to adequately characterize AGN variability.We find that the PSD may be better modelled by

combination of a steep power law of the form 1/f3 onshorter time-scales, and a more shallow power law of the

form 1/f2 on the longer time-scales traditionally probed byground-based variability studies.Author(s): Vishal Kasliwal (Drexel University), Michael Vogeley(Drexel University), Gordon Richards (Drexel University)

221.07 – Observational Tests to DetectPhotometric Reverberation in H-alphaWe present photometric observations of several AGN thatwere secured with the 0.9-m telescope located at the WestMountain Observatory that is operated by Brigham YoungUniversity. The new observations use standard BVR filtersalong with several custom filters that are part of a redshifted H-alpha set. Light curves are presented for severalof the targets along with a summary of the analysis madeto detect lag times between the continuum and broademission line flux as evidence for photometricreverberation. Plans are presented for future research thatwill continue along these lines. We thank the Department ofPhysics and Astronomy along with the College of Physicaland Mathematical Sciences at Brigham Young University forcontinued support of the research work being done at theWest Mountain Observatory.Author(s): Michael Joner (Brigham Young Univ.), Carla Carroll(Brigham Young Univ.)

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221.08 – Three Gamma-ray Active Periods inthe Quasar PKS1510-089 and theirConnection with the Parsec Scale JetBehaviorSince the start of Fermi Large Area Telescope operations in2008 August, the quasar PKS1510-089 has undergone threeperiods of high gamma-ray activity - in 2009, 2011, and2013 - with different amplitudes and complex structure ofgamma-ray outbursts. We analyze the parsec scale jetstructure of the quasar with a resolution of 0.1milliarcseconds using 68 epochs of Very Long BaselineArray (VLBA) observations at 43 GHz from 2007 June to2014 January. We find that the innermost jet ofPKS1510-089 during a quiescent state consists of acompact core and a stationary feature $\sim$0.5 mas fromthe core. During the 2009 and 2011 gamma-ray outbursts,two superluminal knots appeared in the jet for each event,while during the 2013 outburst only one knot was detected.The knots moved down the jet at different apparent speeds,ranging from 23c to 13c. Extrapolated epochs of thepassage of the knots through the core coincide within1\sigma uncertainty with peaks of the gamma-ray lightcurve. We explain the complex structure of the outbursts asthe result of propagation of blobs of relativistic plasma fromthe broad line region to the mm-wave core of the jetthrough a non-uniform field of external photons, with thephysical parameters of the blobs similar to those of thesuperluminal knots seen on the VLBA images. This researchis funded in part by NASA Fermi Guest Investigator grantsNNX11AQ03G and NNX13AO99G.Author(s): Svetlana Jorstad (St. Petersburg University), AlanMarscher (Boston Univ.), Nicholas MacDonald (Boston Univ.), Vishal Bala(Boston Univ.)

221.09 – The Role of Multiple Shocks in theProduction of GeV Gamma-ray Flaring in theBlazar 1156+295As part of work to identify jet conditions during GeV flaringdetected by the Fermi-LAT, we have carried out radiativetransfer modeling of a pair of centimeter-band, total andpolarized flux outbursts in the FSRQ 1156+295 from theUMRAO data archive. The modeling incorporatespropagating shocks and uses the observed spectralevolution between 14.5 and 4.8 GHz as constraints. Thetwo outbursts are nearly identical in amplitude, spectrumand duration. However, the centimeter-band outburstpeaking in 2010.75 is temporally associated with a series ofGeV flares extending over nearly 300 days with peakphoton flux exceeding 10^{-6} photons/cm^2/s, while thecentimeter-band outburst which commenced in earlyAugust 2008 is temporally associated with a well-definedgamma-ray quiescent state. Our analysis reveals that theshocks in the parsec-scale jet during the two events have asimilar sense (forward), orientation (transverse) andcompression, but in the case of the orphan radio-band flareonly 2 shocks were required to reproduce the light curves,while in the event with a paired gamma-ray flare, 4 shockswere required. VLBA imaging of the inner jet at 43 GHzidentifies a single jet component during the orphan flareand complex structure in the later event. This suggests thatdifferences in shock structure, and associated shockinteractions, play a role in the production of gamma-rayflares. This work was supported in part by Fermi GI grantsNNX11AO13G, and NNX13AP18G (U. Michigan) andNNX11AQ03G (Boston U.). T. H. was supported in part by agrant from the Jenny and Antti Wihuri foundation and bythe Academy of Finland project number 267324.Author(s): Margo Aller (Univ. of Michigan), Philip Hughes (Univ. ofMichigan), Hugh Aller (Univ. of Michigan), Talvikki Hovatta (CaliforniaInstitute of Technology), Svetlana Jorstad (Boston University), AlanMarscher (Boston University), Venkatessh Ramakrishnan (Aalto UniversityMetsähovi Radio Observatory)

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221.10 – The Low End of the ElectronSpectrum in Relativistic JetsThere are two problems related to the low end of therelativistic electron spectrum in extragalactic jets that canbe addressed with low radio frequency observations witharcsec resolution. The first is a test of the beamed inverseCompton model (IC/CMB) for the X-ray emission fromquasar jets. Synchrotron emitting electrons with Lorentzfactors of gamma in the range of 50-400 are thoseresponsible for IC/CMB X-ray emission so it is generallynecessary to make a blind extrapolation to very low radiofrequencies from the arcsec resolution data predominantlyobtained at cm wavelengths. The second issue relates topredictions of shock acceleration models that suggest therecould be a low energy break in the electron distributionaround gamma ~ 2000, i.e. at an energy where theelectron momentum is comparable to that of a proton.Intensities and spectral shapes near 100 MHz willsignificantly reduce the required extrapolation and provideevidence for or against the conflicting expectations: asingle power law extending down to gamma ~ 100 versus abreak near gamma=2000. In order to interpret theobservations that will be forthcoming from LOFAR andeventually with SKA, it is necessary to understand theuncertainties affecting the determination of the magneticfield strength in the emitting region, the key factor inassociating a frequency with gamma. In this contributionwe examine the factors involved in computing theequipartition field and argue that invoking parameters thatminimize B(eq) will provide an upper limit to gammacorresponding to an observed frequency. We brieflydescribe a LOFAR observation scheduled for May 2014which will represent a first step in constraining the low endof the electron spectrum. This work was partially supportedby NASA grant GO3-14106X.Author(s): D. Harris (SAO), Teddy Cheung (NRL), L. Godfrey (ASTRON)

221.11 – High Density Optical Observationsof PKS 0558-504PKS 0558-504 is a radio-loud Narrow Line Seyfert 1 with anSED that resembles that of a blazar. We present threenights of high density optical observations. Theseobservations will be put into an historical perspective usingliterature to produce a long-term light curve.Author(s): Amy Campbell (Georgia Gwinnett College)

221.12 – Measuring Supermassive BlackHole Spins in NGC 1365 and MCG--6-30-15Using XMM-Newton and NuSTARWe report on detailed spectral modeling of the Seyfert 1AGN NGC 1365 and MCG--6-30-15 using simultaneous,broadband X-ray spectra from XMM-Newton and NuSTAR.Both of these galaxies show evidence for relativisticreflection from the inner accretion disk in addition tocomplex, variable absorption. The high signal-to-noiseacross the 0.2-79 keV energy band enabled by theseobservations allows us to definitively disentangle thespectral signatures of the continuum, warm and coldabsorption, and reflection from the torus and the inner diskin both sources. These deep pointings also enable the useof time-resolved spectral fitting in order to assess the roleof each component in driving the spectral and temporalvariability of the AGN. This type of analysis allows us toisolate the relativistic reflection signatures in each object,facilitating the most accurate, precise constrains everobtained on the spins of their supermassive black holes.Author(s): Laura Brenneman (Harvard-Smithsonian Center forAstrophysics), Andrea Marinucci (Universita Roma Tre), Dom Walton(California Institute of Technology), Guido Risaliti (INAF/Arcetri), GiorgioMatt (Universita Roma Tre), Fiona Harrison (California Institute ofTechnology), Daniel Stern (California Institute of Technology)

Contributing teams: The NuSTAR team

221.13 – The AGN Corona and SupermassiveBlack Hole of NGC 4151 as Revealed byNuSTAR and SuzakuThrough timing and spectral analyses of simultaneous, 150ks Nuclear Spectroscopic Telescope Array (NuSTAR) andSuzaku X-ray observations of the Seyfert 1.5 galaxy NGC4151, we disentangle the continuum, reflection, andabsorption properties of the innermost regions of the activegalactic nucleus (AGN). Utilizing NuSTAR's broadband (3-79keV) X-ray sensitivity and Suzaku's CCD energy resolutionfrom 0.7-10 keV, we robustly determine properties of theAGN corona and supermassive black hole (SMBH). Weconstrain the coronal temperature and optical depth to be

kTe = 44-29+9 keV and ?=1.4-0.3+2.0, respectively,assuming a coronal slab geometry. Additionally, wedetermine the dimensionless spin, a?0.99, of the SMBH inNGC 4151 for the first time through a spectral analysis.Finally, we show evidence that the coronal flux varies ontime-scales as short as four hours. We discuss constraintsour results put on the coronal geometry. To robustly test forthe presence of relativistic reflection from the inneraccretion disks of Seyfert 1 AGNs, we develop a library oftime-dependent spectra and light curves from simulatedeclipses of an accretion disk by clumpy, absorbing materialcovering a large range of disk, black hole, and absorberparameters. When applied to a high signal-to-noiseobservation of a Compton-thick eclipse of the accretiondisk, these simulations will enable observational tests forthe presence of inner accretion disk reflection in Seyfert 1AGN emission using current X-ray observatories andstandard X-ray data analysis software.Author(s): Mason Keck (Boston University), Laura Brenneman(Harvard-Smithsonian Center for Astrophysics), Martin Elvis (Harvard-Smithsonian Center for Astrophysics), Felix Fuerst (California Institute ofTechnology), Grzegorz Madejski (Stanford Linear Accelerator Center),Giorgio Matt (Università Roma Tre), Fiona Harrison (California Institute ofTechnology), Daniel Stern (California Institute of Technology), JonathanMcDowell (Harvard-Smithsonian Center for Astrophysics), Guido Risaliti(INAF – Osservatorio Astrofisico di Arcetri)

Contributing teams: The NuSTAR Team

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221.14 – The Interplay of the NIR to UVSpectral Energy Distributions ofGamma-Ray Bright BlazarsThe small fraction of AGN in which a relativistic jet isaligned with the observer’s line of sight are classified asblazars. Radiation from the accretion disk and perhaps thejet is absorbed and reprocessed through various structuresinside the AGN, and subsequently re-emitted across abroad range of frequencies. In some blazars, relativelyunprocessed radiation from the accretion disk is visible inthe optical-UV portion of the spectrum. In spectral energydistributions (SEDs) this produces the so-called Big BlueBump (BBB). Measuring the strength of the BBB emission iscomplicated by the fact that the synchrotron emission fromthe relativistic jet is also prominent in the same portion ofthe SED. We separate the unpolarized BBB emission of asample of blazars from the polarized synchrotron emissionpresent in the optical-UV emission through the usespectropolarimetric observations spanning ?= 4000-7000 ?in the observer’s frame. With the assumption that the BBBemission is unpolarized, the spectral index of thesynchrotron emission, ?s, is determined from the polarizedflux spectrum. The strength of the BBB then follows by

fitting a two component model of the form F? = A ???s + B

???BBB , where ?BBB is the spectral index of the BBB and isset to 5/3. We combine these observations with a timeseries of photometric observations spanning the NIR (J, H,and Ks ) and the optical (u? , g? , r? , i? , and z? ) spectrum.This yields a time baseline of several years for a sample ofgamma-ray bright blazars to determine the variability ofthe BBB and to trace its impact on both the NIR emissionfrom the torus, as well as any effect on gamma-rayproduction. Any such variability indicates that the structureof the accretion disc evolves appreciably on time scales offew years. Coupling of BBB emission with dust emission willhelp determine the size scale of the inner-most radius ofthe torus. This is needed to determine the radiationenvironment of the torus and and thereby constrain inverseCompton models for gamma-ray production. This researchis supported in part by NASA Fermi Guest Investigatorgrants NNX11AQ03G and NNX11AO40G and by NSF GK12GLACIER DGE-0947950.Author(s): Michael Malmrose (Boston Univ.), Alan Marscher (BostonUniv.), Svetlana Jorstad (St.Petersburg State University)

221.16 – Optical Spectroscopy of theRestarting Radio Galaxy 3C 219We are investigating the mechanism for the triggering radiojet formation in active galactic nuclei (AGNs). The radiosource 3C 219 appears to have both an ancient remnantlobe system and a small recently-initiated jet. Oneinterpretation of this unusual structure is that the AGN wasactive in the distant past, went dormant, and is nowforming jets again. Thus 3C 219 provides an opportunity tostudy the mechanism of jet formation in a very youngobject. One hypothesis for triggering jet formation in anAGN is gravitational interaction with another galaxy. Thisinteraction should leave traces of optical activity such asenhanced star formation in the host galaxy of the AGN.Optical spectroscopy is used to study the radiation fromionized gas which tells about the physical conditions in thehost galaxy of 3C 219. We have produced spectra of 3C 219and the comparison galaxy B1213+422, and are examiningthe differences between these two fields. Preliminaryresults show little evidence of recent star formation in 3C219.Author(s): Kathryn Weil (Brandeis University), David Roberts(Brandeis University)

221.17 – Modeling the ReverberationResponse of the Dusty Torus Emission fromAGNThe obscuring circum-nuclear torus of dusty molecular gasis one of the major components of AGN (active galacticnuclei), yet its size, composition, and structure are not wellunderstood. These properties can be studied by analyzingthe time response of the dust emission from the torus withrespect to variations in the AGN continuum luminosity; atechnique known as reverberation mapping. Aninternational campaign to monitor 12 Type 1 AGN using theSpitzer Space Telescope and several ground-basedtelescopes has recently been completed. These dataprovide a unique set of well-sampled mid-infrared (IR; 3.6,4.5 microns) and optical (B, V bands) light curves over atwo-year baseline, which will be used to determineapproximate sizes of the tori for these galaxies. To helpextract structural information contained in the data we arealso developing a computer model that simulates thereverberation response of a clumpy torus for directcomparison with the observed IR light curves. Here Ipresent preliminary results from these simulations andcompare them to the light curves of NGC 6418, one of the12 galaxies observed during the Spitzer campaign.Author(s): Triana Almeyda (Rochester Institute of Technology),Andrew Robinson (Rochester Institute of Technology), Michael Richmond(Rochester Institute of Technology), Billy Vazquez (Rochester Institute ofTechnology)

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221.18 – Time-dependent Photoionization ofGaseous Nebulae: Time-dependent Versionof XSTARIn a previous paper we developed a code to study theproblem of time-dependent photoionization of purehydrogen gaseous nebulae subjected to sudden changes inthe intensity of ionizing radiation. We have showed thatchanges in the ionizing radiation yield ionization/thermalfronts that propagate through the cloud creating largepressure imbalances with important dynamical effects inthe cloud. Now we present a full time-dependent version ofthe XSTAR code to solve the energy balance, ionizationbalance, and radiation transfer equations in aself-consistent fashion in nebulae subjected to rapidlychanging ionizing radiation. We compare the results of theprevious paper of the simplified hydrogen model to that ofthe current full atomic model. Further, we investigatetime-dependent ionization effects in Quasar BroadAbsorption Line (BAL) clouds.Author(s): Ehab Elhoussieny (Western Michigan University), ManuelBautista (Western Michigan University), Timothy Kallman (NASA GoddardSpace Flight Center), Javier Garcia (Harvard-Smithsonian Center forAstrophysics)

221.19 – Time-variable Linear Polarizationas a Probe of the Compact Jets of BlazarsA single measurement of linear polarization of anonthermal source provides direct information about themean direction and level of ordering of the magnetic field.Monitoring of the polarization in blazars, combined withmillimeter-wave VLBI imaging in both total and polarizedintensity, has the potential to determine the geometry ofthe magnetic field. This is a key probe of the physicalprocesses in the relativistic jet, such as ordered fieldcomponents, turbulence, magnetic reconnections,magnetic collimation and acceleration of the jet flow,particle acceleration, and radiative processes that produceextremely luminous, highly variable nonthermal emission.The authors will show some examples of well-sampledmonitoring observations of multi-waveband flux and radio-optical polarization of blazars. In some cases, the observedpolarization patterns appear systematic, while in othersrandomness dominates. Explanations involve helicalmagnetic fields, turbulence, and perhaps particleacceleration that depends on the angle between themagnetic field and shock fronts that might be present. Thisresearch is supported in part by NASA through Fermi GuestInvestigator grants NNX11AQ03G, NNX12AO79G, andNNX13AP06G to Boston U., NNX12AO93G to Steward Obs.,and RFBR grants 12-02-00452 and 12-02-31193 to St.Petersburg State U.Author(s): Alan Marscher (Boston University), Svetlana Jorstad (St.Petersburg State U.), Valeri Larionov (St. Petersburg State U.), Ivan Agudo(JIVE), Paul Smith (Steward Obs.)

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222 – Evolution of Galaxies PostersPoster Session – Essex Ballroom and America Foyer – 03 Jun 2014 09:00 AM to 06:30 PM

222.01 – HIghMass – High HI Mass, HI-richGalaxies at z~0 (Sample Definition, Opticaland H? Imaging, and Star FormationProperties)We present first results of the study of a set of exceptionalHI sources identified in the 40% ALFALFA extragalactic HIsurvey catalog ?.40 as being both extremely HI massive

(MHI > 1010 M?) and having high gas fractions for theirstellar masses: the HIghMass galaxy sample. We analyzeUV- and optical- broadband and H? images to understandthe nature of their relatively underluminous disks in opticaland to test whether their high gas fractions can be trackedto higher dark matter halo spin parameters or late gasaccretion. Estimates of their star formation rates (SFRs)based on SED-fitting agree within uncertainties with the H?luminosity inferred current massive SFRs. The HII region

luminosity functions, parameterized as dN/dlogL ? L?, havestandard slopes at the luminous end (? ~ ?1). The globalSFRs demonstrate that the HIghMass galaxies exhibit activeongoing star formation (SF) with moderate SF efficiency,but relative to normal spirals, a lower integrated SFR in thepast. Because the SF activity in these systems is spreadthroughout their extended disks, they have overall lowerSFR surface densities and lower surface brightness in theoptical bands. Relative to normal disk galaxies, the majorityof HIghMass galaxies have higher H? equivalent widths andare bluer in their outer disks, implying an inside-out diskgrowth scenario. Downbending double exponential disksare more frequent than upbending disks among thegas-rich galaxies, suggesting that SF thresholds exist in thedownbending disks, probably as a result of concentratedgas distribution. Future observations of the HIghMassgalaxies will study the HI-to-H2 transition and the empiricalKennicutt-Schmidt (KS) relation in more detail to explorehow such massive HI disks can exist without havingconverted the bulk of gas into stars yet.Author(s): Shan Huang (Cornell University), Martha Haynes (CornellUniversity), Riccardo Giovanelli (Cornell University), Gregory Hallenbeck(Cornell University), Michael Jones (Cornell University), Elizabeth Adams(Cornell University), Jarle Brinchmann (Sterrewacht Leiden), JayaramChengalur (National Centre for Radio Astrophysics), Leslie Hunt (INAF-Osservatorio Astrofisico di Arcetri), Karen Masters (Institute of Cosmologyand Gravitation, Portsmouth), Satoki Matsushita (ASIAA), Amelie Saintonge(University College London), Kristine Spekkens (Royal Military College ofCanada)

222.02 – Merger Signatures in the GalaxyCluster Abell 98We present results from Chandra and XMM-Newtonobservations of the galaxy cluster Abell 98 (A98), whichshows three major components: a relatively brightsubcluster to the north (A98N), a disturbed subcluster tothe south (A98S), and a fainter subcluster to the far south(A98SS). We find evidence of a surface brightness andtemperature asymmetry in A98N that is consistent with thepresence of a leading bow shock to the south, created byan early stage merger between A98N and A98S. We alsofind that A98S has an asymmetric temperature structure inthe core, likely due to a separate ongoing merger. Evidencefor this is also seen in the optical data. A98S hosts awide-angle tail (WAT) radio source powered by a centralactive galactic nucleus (AGN). We find evidence for a cavityin the intracluster medium (ICM) that has been evacuatedby one of the radio lobes, suggesting that AGN feedback isoperating in this system. The three main subclusters liealong a line in projection, suggesting the presence of alarge scale filament. We observe an excess of emissionalong the filament between A98N and A98S, but a surfacebrightness profile shows that this excess emission isconsistent with the overlap of the extended gas haloes ofA98N and A98S. We find that the temperature of this regionis consistent with the temperature of the gas at similar radiioutside this bridge region. Lastly, we examine the clusterdynamics. We find that A98N and A98S are likely bound toone another, with a 67% probability, while A98S and A98SSare not bound at a high level of significance.Author(s): Rachel Paterno-Mahler (Center for Astrophysics), ScottRandall (Center for Astrophysics), Esra Bulbul (Center for Astrophysics),Felipe Santos (Center for Astrophysics), Christine Jones (Center forAstrophysics), Stephen Murray (Johns Hopkins University), ElizabethBlanton (Boston Univ.), Ryan Johnson (Gettysburg College)

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222.03 – 3C28 in Abell 115- A Radio SourceWith a Twist: Tracing Gas Vortices in aMerging Subcluster CoreAbell 115 is one of the “bimodal” clusters, first identifiedfrom Einstein Observatory X-ray images. The X-ray image isdominated by emission from two subclusters, separated byabout 900 kpc, that are in the process of merging. Thenorthern subcluster (A115-N) contains a bright centralgalaxy that hosts the radio source 3C28. 3C28 has aremarkable morphology. Although there is no evidence of apresently active nucleus, there are two prominent jetsconnected to a pair of radio lobes, each of which exhibits aradio tail. A115-N shows a classic cold front, the remarkablephenomenon first studied from Chandra clusterobservations. We describe the overall structure of thecluster from detailed Chandra obserations. In addition, weexploit the Chandra data and the cold front phenomenon tostudy the gas motions in and around A115-N that hosts3C28. The subcluster motion of A115-N through the clusterinduces counter-rotating vortices in the subcluster gas thatgive rise to the unique radio morphology of 3C28 with itstwo radio tails pointing in the direction of motion of A115-N.Thus, the radio emitting plasma acts as a dye in a fluidtracing the vortices in the X-ray emitting gas, resemblingtext book pictures of fluid motions.Author(s): William Forman (SAO), Eugene Churazov (IKI), SebastianHeinz (University of Wisconsin), Simona Giacintucci (University ofMaryland), Christine Jones (SAO), Akos Bogdan (SAO), Laurence David(SAO), Ralph Kraft (SAO), Matteo Murgia (OAC-INAF), Maxim Markevitch(GSFC), Scott Randall (SAO), Reinout Van Weeren (SAO), Alexey Vikhlinin(IKI)

222.04 – K-band Polarimetry of NGC 891We present the first K-band (2.2 um) polarimetryobservations of the edge-on galaxy NGC 891. Near-infrared(NIR) polarimetry reveals the plane-of-sky projectedmagnetic (B) field orientations in dusty, star-forminginterstellar media. Previous optical wavelength polarimetryof NGC 891 found predominantly disk-perpendicularpolarizations (Scarrott & Draper 1996) while H-bandpolarimetry revealed mostly disk-parallel polarizations withan interesting 15 degree offset from the major axis positionangle (Jones 1997; Montgomery & Clemens 2014). InH-band, Montgomery & Clemens also detected the first NIRpolarization null-point, located about 5 kpc northeast ofNGC891's center. It may be related to the polarizationnull-points predicted by Wood (1997) and modeled by Wood& Jones (1997). At the longer K-band wavelength, thesenew observations better reveal B-field orientation changesin the disk. The Wood (1997) radiative transfer polarizationmodel predicted null-point location changes withwavelengeth. We will use the new K-band polarimetry,along with our H-band polarimetry, to test this prediction. Ifthe null-point location does not depend on wavelength,then the null-point may instead be due to spiral armaligned B-fields (e.g., Fletcher et al. 2011). This researchwas supported through NSF grant AST 09-07790.Author(s): Jordan Montgomery (Boston University), Dan Clemens(Boston University)

222.05 – Unraveling ICM Physics and AGNFeedback with Deep Chandra X-rayObservations of the Galaxy Group NGC 5813We present results from deep (650 ks) Chandra X-rayobservations of the galaxy group NGC 5813. This systemshows three pairs of colinear cavities, with each pairassociated with an elliptical AGN outburst shock. Due to therelatively regular morphology of this system, and theunique unambiguous detection of three distinct AGNoutburst shocks, it is particularly well-suited for the study ofkinetic mode AGN feedback and the AGN outburst history.Topics presented include results on the role of shockheating in AGN feedback, feedback as a solution to thecooling flow problem, the variability of the AGN outburstpower over long timescales, and constraints on themicrophysics of the ICM.Author(s): Scott Randall (Harvard-Smithsonian Center forAstrophysics), Paul Nulsen (Harvard-Smithsonian Center forAstrophysics), Tracy Clarke (Naval Research Lab), William Forman(Harvard-Smithsonian Center for Astrophysics), Christine Jones (Harvard-Smithsonian Center for Astrophysics), Ralph Kraft (Harvard-SmithsonianCenter for Astrophysics), Elizabeth Blanton (Boston University)

222.06 – A study of the temporal behaviorof the X-ray Sources in the Galaxy NGC 1232over a three year periodThe Galaxy NGC 1232 has been observed using theChandra X-ray Observatory over a three year period withsamples ranging from 50 ks to up to three years. Most ofthe X-ray sources are found to be variable, with some onlyappearing in one of the five observations taken over thethree years. The problem of source confusion withbackground quasars will be discussed. This work wassupported by Contract SV2-82024 from the SmithsonianAstrophysics Observatory to the Huntingdon Institute forX-ray Astronomy, LLC.Author(s): Gordon Garmire (Huntingdon Institute for X-rayAstronomy, LLC), Audrey Garmire (Huntingdon Institute for X-rayAstronomy, LLC)

222.07 – Photometric Profiles of NearbyEarly-Type Galaxies Using SDSSThe outer regions of galaxies provide information abouttheir assembly histories. We are carrying out a detailedanalysis of the Sloan Digital Sky Survey (SDSS) photometricprofiles of a large sample of nearby early-type galaxies, inorder to look for transitions between their inner and outerproperties. Here we present initial results from this survey.Author(s): Beth Johnson (San Jose State University), AaronRomanowsky (University of California Observatories)

222.08 – A New Search for Ultra-CompactDwarfsUltra-compact dwarfs (UCDs) are a recently discoveredclass of object that consists of high stellar densities in aradius of around 10 to 40 pc. We are searching for UCDsaround local galaxies using the SDSS database, withspectroscopic follow. We present initial results of our surveyincluding a discovery of a unique and interesting object.Author(s): Richard Vo (San Jose State University), AaronRomanowsky (University of California Observatories), Jay Strader (MichiganState University), Charlie Conroy (University of California - Santa Cruz),Mark Norris (Max Planck Institute for Astronomy), Jean Brodie (University ofCalifornia Observatories)

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222.09 – Gas-phase metallicity of void dwarfgalaxiesWe study how the cosmic environment affects galaxyevolution in the Universe by comparing the metallicities ofgalaxies in voids with similar-sized galaxies in more denseregions. Ratios of the fluxes of emission lines, particularlythose of the forbidden [OIII] and [SII] transitions, provideestimates of a region's electron temperature and numberdensity. From these two quantities and the emission lineintensities, we estimate the abundance of oxygen with theDirect Te method. We estimate the metallicity of 19 voiddwarf galaxies and 35 wall dwarf galaxies using data fromSDSS via the MPA-JHU value-added Garching catalog. Wefind very little difference between the two sets of galaxies,indicating little influence from the large-scale environmenton stellar evolution. Of particular interest are a number ofextremely metal-poor dwarf galaxies.Author(s): Kelly Douglass (Drexel University), Michael Vogeley(Drexel University)

222.10 – The HI Content of Galaxies inGroups as Measured by ALFALFAWe present the HI content of galaxies in a sample of elevenwell-studied groups in the Arecibo Legacy Fast-ALFA(ALFALFA) survey. Specifically, we compare the HIdeficiency, HI mass function, and HI mass fraction forgalaxies in the center 1.5 Mpc of the groups to those forgalaxies in a “field” sample defined as a 2-5 Mpc projectedannulus surrounding each group.Author(s): Mary Crone-Odekon (Skidmore College), RebeccaKoopmann (Union College), Martha Haynes (Cornell University), Rose Finn(Siena College)

Contributing teams: ALFALFA Team

222.11 – Using Chandra X-ray Observationsto Characterize the Planck ESZ Clusters ofGalaxiesThrough the SZ effect, the Planck mission has provided acomplete nearly mass-limited sample of clusters ofgalaxies. Through extensive Chandra X-ray observations ofthe large sample of Planck ESZ clusters at z<0.35, we cancharacterize each cluster in terms of its X-ray luminosity,gas mass, gas temperature, entropy, central cooling time,presence of active AGN, and morphology. We determine thefraction of Planck clusters with different clustermorphological types, ranging from cool core clusters todisturbed major mergers. Examples of each cluster typewill be presented, including cool core clusters, "Coma-like"flat core systems, and "bullet-like" major mergers. We willcompare the fraction of morphological types in the Planck(z<0.35) sample with higher redshift samples.Author(s): Christine Jones (Harvard-Smithsonian, CfA), WilliamForman (Harvard-Smithsonian, CfA), Felipe Santos (Harvard-Smithsonian,CfA)

Contributing teams: Chandra-Planck XVP Consortium

222.12 – Early Type Galaxies in the ChandraCOSMOS surveyWe study a sample of 69 X-ray detected Early Type Galaxies(ETGs), selected from the Chandra COSMOS survey, toexplore the relation between the X-ray luminosity of hotgaseous halos L_(X, gas) and the integrated stellarluminosity (L_K) of the galaxies, in a range of redshiftextending out to z=1.5. In the local universe a tight steeprelationship has been stablished between these twoquantities suggesting the presence of largely virializedhalos in X-ray luminous systems. We use well establishedrelations from the study of local universe ETGs, togetherwith the expected evolution of the X-ray emission, tosubtract the contribution of low mass X-ray binarypopulations (LMXBs) from the X-ray luminosity of oursample. Our selection minimizes the presence of activegalactic nuclei (AGN), yielding a sample representative ofnormal passive COSMOS ETGs; therefore the resultingluminosity should be representative of gaseous halos,although we cannot exclude other sources such asobscured AGN, or enhanced X-ray emission connected withembedded star formation in the higher z galaxies. We findthat most of the galaxies with estimated L_X<10^42 erg/sand z<0.55 follow the local relation. For these galaxies, thegravitational mass can be estimated with a certain degreeof confidence from the local virial relation. However, themore luminous (10^42<L_X<10^43.5 erg/s) and distantgalaxies present significantly larger scatter; these galaxiesalso tend to have younger stellar ages. The divergencefrom the local relation in these galaxies implies significantlyenhanced X-ray emission, up to a factor of 100 larger thanpredicted from the local relation. We discuss theimplications of this result for the presence of hidden AGN,and the evolution of hot halos, in the presence of nuclearand star formation feedback.Author(s): Francesca Civano (SAO), Giuseppina Fabbiano (SAO), SilviaPellegrini (Bologna University), Dong-Woo Kim (SAO), Alessandro Paggi(SAO), Martin Elvis (SAO)

222.13 – ALMA detected overdensity ofsub-mm sources around WISE-selectedextremely red galaxiesWe study a sample of 49 regions around the extremely redWISE-selected galaxies which earlier studies suggest arehyper luminous z~2 AGN sources. They were observed withthe Atacama Large Millimeter/Submillimeter Array in Band7 (345 GHz) down to an rms of ~0.2mJy and 0.5mJy forobservations at 0.5" and 1.2", respectively. We detect atotal of 31 sources with signal to noise higher than 3.5 in 20of the 49 fields. We produce the source counts of thesources located in the primary beam radius (18.1"). Thecounts clearly show an excess compared with previouscounts and models suggesting these sources reside inhighly clustered environments.Author(s): Andrea Silva (Tufts University), Anna Sajina (TuftsUniversity)

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222.14 – Analyzing a High-Redshift GalaxyClusterHow far back in cosmic history clusters of galaxies formedis a major question in extragalactic astronomy. Galaxyclusters make up the largest scale structures of theuniverse. The farthest galaxy cluster currently known is atredshift 1.62 (Papovich, C. et al, 2010), corresponding tonearly 10 billion years ago. We do not yet know if this is theearliest point in time for galaxy clusters or if they go backstill further to the start of the universe 13.7 billion yearsago. A candidate galaxy cluster at redshift 2.3 waspreviously identified through the work of Professor JamesLowenthal of Smith College. Analysis of the emissionspectrum of a quasar at redshift 2.6, QSO PHL 957,revealed a Damped Lyman-alpha Absorber (DLA)- a hugeintervening cloud of neutral hydrogen- at redshift 2.3(Lowenthal et al, 2000). Further observations with theHubble Space Telescope (HST) and other telescopesrevealed 19 emission galaxies associated with the DLAincluding the Coup Fourré Galaxy, a Lyman-alpha emittinggalaxy and 18 other galaxies within 2 Mpc (Lowenthal et al,2010). This strong overdensity is one of the best currentcandidates for a massive, high-redshift, gravitationallybound cluster of galaxies. If these galaxies are at the sameredshift, we should detect strong Lyman-alpha peaks at 400nanometers for each of the 13 galaxies studied. Images ofthe entire cluster, along with spectra for 13 of its 20objects, had been obtained using the Gemini NorthTelescope in 2010. Imaging and spectroscopy wasperformed on this galaxy cluster- resulting in detectedLyman-alpha peaks at 400 nanometers in only 3 galaxies,indicating that these three, at least, are all at redshift 2.3.Also achieved was a clearer, publishable set of spectraalong with a high-quality image of the cluster. We arepresently in the process of completing photometry on thegalaxies, which involves measuring the intensity of emittedlight in various wavelengths. It is possible that we will beable to confirm the redshift for several galaxies bycomparing the measured intensity of light at differentwavelengths coming from these distant galaxies to modelsof what the spectrum should look like if we were at thesource.Author(s): Isabel Lipartito (Smith College), James Lowenthal (SmithCollege)

222.15 – First Spectroscopic Confirmation ofa Monster Galaxy at z=3.3 and DetailedStellar Population and Structural PropertiesWe present the first spectroscopic confirmation of an ultra-massive galaxy at z,phot = 3.3 using data fromKeck-NIRSPEC, VLT-Xshooter, and GTC-Osiris. We detectstrong [OIII] and Ly? emission, and weak [OII], CIV, and HeII,confirming the redshift at z,spec = 3.3512. Modeling theemission-line corrected spectral energy distribution (fromthe Galex UV to IRAC 8 ?m, as well as the binned spectra)results in a best-fit stellar mass of M,stellar =3×10'11M,sun (Kroupa), SFR of a few solar masses peryear, negligible dust extinction, an age of ? 300 Myr, and avery short burst of star formation, setting the formationredshift of this galaxy at z?4. From the analysis of the lineratios and widths, and the observed flux at 24 ?m weconfirm the presence of a luminous AGN, with bolometricluminosity of ? 8 × 10'45erg/s. The non detection in theX-ray data implies a Compton-thick nature for the type-2AGN. Potential contamination of the observed SED from theAGN continuum is constrained, placing a lower limit on thestellar mass of 2 × 10'11M,sun. HST/WFC3 H160 and ACSI814 images were modeled with GALFIT, resulting in a verycompact galaxy (effective radius r,e ? 1 kpc) and a deVaucouleurs’s profile with n?4. This object represents theprototype galaxy of an ultra-massive galaxy that formed atz?4 in a very intense burst, is about to transition toquiescent, and it hosts a very powerful super massive blackhole potentially responsible for the quenching of the starformation activity.Author(s): Zehra Cemile Marsan (Tufts University), Danilo Marchesini(Tufts University)

222.16 – SED Modeling of z~0.3-4IR-Luminous Galaxies Using HydrodynamicSimulationsWe examine a sample of 343 24?m-selected (U)LIRGS withz~0.3-4 using a library of hydrodynamic galaxy mergersimulations. Each galaxy in our sample has Spitzer IRSspectra (the largest non-local sample to date) along withbroadband photometry, including Hershel far-IR data. Thespectra display a large range of relative stellar and AGNcontributions to the infrared spectrum amongst oursources. The simulations, built from GADGET-2hydrodynamic merger simulations processed through theSUNRISE radiative transfer code, span a range of dustproperties, merger stages, AGN strength, and viewingperspectives. By comparing these simulations to ourobserved data we are able to investigate how theunderlying physical conditions of galaxies affect theobserved SEDs, with particular emphasis on the role AGN.Moreover the simulations allow us to investigate the levelof systematic uncertainty, which with traditional methodswould be difficult or impossible.Author(s): Eric Roebuck (Tufts University), Anna Sajina (TuftsUniversity), Alexandra Pope (University of Massachusetts Amherst), AllisonKirkpatrick (University of Massachusetts Amherst), Lin Yan (CaliforniaInstitute of Technology), Christopher Hayward (Max-Planck-Institut fürAstrophysik), Gregory Snyder (Johns Hopkins University), Lars Hernquist(Harvard–Smithsonian Center for Astrophysics)

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222.17 – A Markov Chain Monte CarloSoftware Package to Constrain theEvolution of Luminosity Functions, Test SEDModels, and Simulate Future SurveysWe present a novel simulation and fitting program whichemploys MCMC to constrain the spectral energy distributionmakeup and luminosity function evolution required toproduce a given mutli-wavelength survey. This tool employsa multidimensional color-color diagnostic to determinegoodness of fit, and simulates observational sources oferror such as flux-limits and instrumental noise. Our goalsin designing this tool were to a) use it to study Infrared

surveys and test SED template models, and b) create it insuch a way as to make it usable in any electromagneticregime for any class of sources to which any luminosityfunctional form can be prescribed. I will discuss our specificuse of the program to characterize a survey from theHerschel SPIRE HerMES catalog, including implications forour luminosity function and SED models. I will also brieflydiscuss the ways we envision using it for simulation andapplication to other surveys, and I will demonstrate thedegree to which its reusability can serve to enrich a widerange of analyses.Author(s): Noah Kurinsky (Tufts University), Anna Sajina (TuftsUniversity)

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223 – Young Stellar Objects, Star Formation, and Star Clusters PostersPoster Session – Essex Ballroom and America Foyer – 03 Jun 2014 09:00 AM to 06:30 PM

223.02 – How is kinematic structureconnected to the core scale from filamentscale?; Mopra mapping observations withmulti-lines of dense cores in Lupus IRecently, high sensitivity mappings of nearby molecularclouds in far-infrared and submillimeter wavelengths withHershel and AzTEC/ASTE show ubiquitous existence of thefilamentary structures with 0.1-pc uniform width. It isimportant to investigate dense core formation from largescale structure via fragmentation. We have conductedMOPRA multi-line mapping observations covered on 0.02 -0.2 pc scales of 8 dense cores in a filamentary cloud ofnearby Lupus I at 140 pc. A class 0/I protostellar core IRAS15398-3359 is included as a sample, which has an adjacentprestellar core with the separation of 0.13pc in the west.The maps of N2H+, HNC, HC3N show well associated witheach core. The velocity field of C18O shows 1.4 km/s/pcfrom north to south over the region containing two densecores, which is consistent with past observation of NANTEN.In contrast to C18O results, the velocity field of HC3Nshows different structures, which suggest counter rotationof two dense cores; 1.2 km/s/pc from north-west tosouth-east around a protostellar core and 0.8 km/s/pc fromeast to west around a presteller core. The filament will befragmentized and collapsed to dense cores when the linedensity is over 2Cs/G (where Cs is sound speed and G isgravitational constant). If that velocity gradient was causedby such situation, it should be red-blue-red-blue across twodense cores but the observed kinematics is not consistentwith this scenario, which requires that the filamentstructure would be extremely curved with a skew angle.Although we cannot reject the collapsing interruption, thoseresults suggest the spin-up rotating picture separated fromlarge-scale structure.Author(s): Kazuhiro Kiyokane (National Astronomical Observatoryof Japan), Masao Saito (National Astronomical Observatory of Japan),Kengo Tachihara (Nagoya University), Kazuya Saigo (National AstronomicalObservatory of Japan), Tim van Kempen (Leiden Observatory), PauloCortes (Joint ALMA Observatory), Tracey Hill (Joint ALMA Observatory),Lewis Knee (Joint ALMA Observatory), Yasutaka Kurono (NationalAstronomical Observatory of Japan), Satoko Takahashi (NationalAstronomical Observatory of Japan), Higuchi Aya (National AstronomicalObservatory of Japan), Lars-Ake Nyman (Joint ALMA Observatory)

Contributing teams: SOLA team

223.03 – Multiplicity study of Herbig Ae/BestarsWe present the results of a high resolution imaging surveyto study the multiplicity of Herbig Ae/Be stars. 143 starswere observed with Adaptive Optics imaging, during twoseparate periods: 1993-1996 and 2005-2007. A total of 248companions were detected, around 87 primary stars. 69system were found to be likely true multiple systems,based on a statistical analysis. A complementary study forthose stars for which multi-epoch data exists, confirms theresults for almost all of the stars of this subset providingtheir proper motion is large enough and the multi-epochdata spanned a long enough time period.Author(s): Nicole Van Der Bliek (CTIO/NOAO), Sandrine Thomas(NASA Ames Research Center), Bernadette Rodgers (Gemini), JeromeBouvier (Observatoire de Grenoble), Claudia Araya (NASA Ames ResearchCenter), Greg Doppmann (Keck Observatory), Maria Cordero (IndianaUniversity)

223.04 – Spitzer Observations of theEclipsing T Tauri System KH15DWe present 3.6 micron and 4.5 micron photometry of thebinary T Tauri system KH15D obtained with the SpitzerSpace Telescope. The data cover the full range of phases ofthis eclipsing system. Its components have spectral typesK7 (Star A) and K1 (Star B) and an orbital period ofapproximately 48 days. Models suggest that a precessingcircumbinary ring is responsible for the eclipses. The ring isinclined with respect to the binary orbit and the stars “rise”and “set” with respect to its sharp edge during each cycle.The system’s colors show distinct reddening when it is in itsfaint phase and the degree of reddening exceeds what isexpected from just the stars. One explanation for theexcess is a young, luminous giant planet orbiting beyondthe outer edge of the ring. We consider this hypothesis aswell as the possibility that the excess radiation comes fromdisk emission or from reddening. If reddening is implicatedthe size of the grains must be of the order of 5 microns orlarger. We are grateful to J. Stauffer and the CSI 2264 teamfor their assistance with this project.Author(s): Nicole Arulanantham (Wesleyan University), WilliamHerbst (Wesleyan University), Ann Marie Cody (Spitzer Science CenterCalifornia Institute of Technology)

Contributing teams: CSI 2264 Team

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223.05 – Characterizing YSO EvolutionaryStates from their Mid-Infrared ColorsNear and mid-infrared (NIR/MIR) colors have long beenused to identify young stellar objects (YSOs) for furtherstudy. For example, the NIR/MIR spectral energydistributions (SEDs) are used to classify the YSOs intoclasses or stages that signify the relative amounts of massin the YSO envelopes and disks, from massive thickenvelopes down to essentially no remaining envelope butstill the presence of a disk. The extension of the SEDs tofar-infrared (FIR) wavelengths has enabled much betterestimates of the luminosity, the mass in the YSO envelopes,the accretion rates, and some estimate of the ages of theYSOs through the use of Monte Carlo radiation transfermodels. However, further details about the envelopes anddisks of the YSOs required spectra, either IR or radio. Infact, basic information about the composition of theenvelopes is also available from the YSO colors asmeasured by Spitzer's Infrared Array Camera (IRAC). In thisposter we demonstrate how the presence of either ices inthe envelopes or PAHs in the outflow regions substantiallychanges the observed colors away from the locus of themajority of observed red objects. The reason is that iceabsorption features decrease the fluxes in the IRAC 3.6, 5.8,and 8.0 micron bands much more than in the 4.5 micronband, leaving the 4.5 micron band comparatively bright.This is shown in the [3.6]-[4.5] vs [4.5]-[5.8] color-colorplot, where the icy-envelope YSOs and the PAH-emittingYSOs fall on very different loci from other dusty objects.Visually, candidate icy-envelope YSOs can be detected byplotting IRAC images with red, green, and blue colors usedfor the IRAC 5.8, 4.5, and 3.6 micron bands: the YSOs withicy envelopes stand out has having a distinct yellow color incontrast to blue stars and red YSOs whose MIR spectra aredominated by PAH emission and sometimes the forbiddenlines of a massive YSO close to the main sequence. Weinterpret the presence of icy envelopes as indicating thecentral protostar has not evolved to a high enoughtemperature to evaporate the ice or excite the PAHs.Confirmation of YSO candidates should be obtained fromthe FIR SED. Applications include estimating theevolutionary status of the YSOs found in FIR surveys.Author(s): Janet Simpson (SETI Institute), Angela Cotera (SETIInstitute), Barbara Whitney (Space Science Institute)

223.06 – Radio Recombination Line andContinuum Emission from Flickering UC HIIRegions in Sgr B2 MainWe have observed the Galactic Center star forming regionsSgr B2 Main and North at 1.3 cm and 7 mm with the VLAover a 23 year time baseline. The 1.3 cm observations, at aresolution of ~0.25", indicate that 4 of the 41 ultracompactsources in Sgr B2 Main and North have experiencedsignificant changes in flux density between 1989 and 2012,with three sources brightening (F10.303, F1 and F3) andone source fading (K3). We present a summary of theseresults, as well as new 7 mm continuum images of Sgr B2Main and North. Finally, we present the first high spectralresolution radio recombination line (RRL) observations ofthe sources with detected flux density changes.Author(s): Christopher De Pree (Agnes Scott College), RobertoGalvan-Madrid (ESO), Miller Goss (NRAO), Eric Keto (Harvard-SmithsonianCfA), Ralf Klessen (Institut f\"{u}r Theoretische Astrophysik),Mordecai-Mark Mac Low (American Museum of Natural History), ThomasPeters (Institut f\"{u}r Theoretische Physik), Ashley Monsrud (Agnes ScottCollege), David Wilner (Harvard-Smithsonian CfA)

223.07 – Clustering Properties of YoungStellar Objects in the Massive Star FormingRegion W49Massive stars play a vital role in the star formation process,yet their own formation and their effects on subsequentgenerations of star formation is not well understood. Toimprove our understanding, we have begun a detailedstudy of massive and active star forming complexes ingiant molecular clouds outside the Galactic Center. One ofthe main goals of this study is to identify and classify theYoung Stellar Objects (YSOs) in each region by using SpitzerSpace Telescope IRAC & MIPS data. Following this,YSOclusters will be identified based on spatial distributions ofthe detected sources. Studying clusters with differentevolutionary stages will help us to understand theformation and evolution processes from beginning to end.This study will also provide significant information on howmassive stars interact with their environment and how theyaffect the low-mass star formation in the cloud. Within thiscontext, we present the initial results of our investigationon the star-forming complex W49 that is one of theyoungest, most luminous and most massive star formationregion in the Galaxy. We used a combination of SpitzerSpace Telescope IRAC & MIPS data, Two Micron All SkySurvey (2MASS) and UKIRT Deep Infrared Sky Survey(UKIDSS) data to identify and classify the Young StellarObjects (YSOs) and generated a final catalog with aphotometry of sources containing more than 2 millionsources within an area of size ?lx?b = 2°.6 x 3°.4, centeredat (l,b) = (42°.7,0°.04) over a wavelength range from 1.2 to24 ?m. With a preliminary source classification we identifiedthousands of YSO candidates. In addition, to understandthe evolution of star formation in W49 we analyzed thedistributions of YSOs to identify the clusters based onspatial distributions of the detected sources.Author(s): Gozde Saral (Istanbul University), Joseph Hora (Harvard-Smithsonian Center For Astrophysics), Xavier Koenig (Yale University), TalatSaygac (Istanbul University)

223.08 – The Study of tidal strippingsubstructures around four metal-poorglobular clusters in the Galactic bulgeWe have investigated the stellar spatial density distributionaround four metal-poor globular clusters (NGC 6266, NGC6626, NGC 6642, and NGC 6723) in the Galactic bulgeregion, by using 45’×45’ wide-field J, H, and K imagesobtained with WFCAM detector on the United KingdomInfrared Telescope. In order to minimize the field starcontamination and identify the cluster’s member candidatestars, we used a statistical filtering algorithm and thenweighted the stars on the color-magnitude diagram. Intwo-dimensional stellar density maps, we found that thespatial density distribution of stars around four globularclusters is asymmetric and show tidal stripping features.The orientation of tidal substructure seems to associatewith the effect of dynamical interaction with the Galaxy andthe cluster’s space motion. Indeed, the radial surfacedensity profile accurately describes this striping structureas a break in the slope of profile. We expect that ourobservational results could give us further constraints tounderstand the evolution of clusters as well as mergingscenario of the formation of the Galaxy.Author(s): Sang-Hyun Chun (Yonsei University Observatory),Minhee Kang (Department of Astronomy, Yonsei University), Young-JongSohn (Department of Astronomy, Yonsei University)

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223.09 – Globular Cluster MembershipProbabilities from All-Sky Proper MotionCatalogsRecent all-sky catalogs such as UCAC4 (Zacharias et al.2013, AJ, 145:44) and PPMXL (Roeser et al. 2010, AJ, 139,2440) contain proper motions with errors of 1-10 mas/yr.This precision is sufficient to determine membershipprobabilities for stars in the fields of globular clusters if thecluster motion is reasonably different from the field starmotion. We use membership probabilities for stars in thefield of the globular cluster NGC 6397 derived from veryhigh precision relative proper motions (~ 0.2 mas/yr errors)from long-focus plates to test membership probabilitiesderived from UCAC4 and PPMXL motions. We also explorethe use of UCAC4 and PPMXL to search for cluster membersbeyond the small field of the long-focus plates. Thispublication makes use of data products from the Two MicronAll Sky Survey, which is a joint project of the University ofMassachusetts and the Infrared Processing and AnalysisCenter/California Institute of Technology, funded by NASAand the NSF. This research has made use of the VizieRcatalogue access tool, CDS, Strasbourg, France. Thisresearch has been partially supported by the NSF.Author(s): Richard Rees (Westfield State University), Kyle Cudworth(Yerkes Observatory, The University of Chicago)

223.10 – Ruprecht 147: Dating middle-agedstarsRuprecht 147 is the oldest nearby star cluster, with an ageof 3 Gyr and distance of 300 pc, which allows R147 to serveas a sorely needed intermediate-aged benchmark. Stellarages are difficult to infer for main sequence stars, but agecan reveal itself through the spin down of stars viamagnetic braking, which also causes magnetic activity towane with time. We have present results of our studies ofthe magnetic activity and rotation of FGK stars. We alsohope to have newly identified M dwarf members by thetime of this meeting, and will discuss their activity,manifested in chromospheric H-alpha emission.Author(s): Jason Curtis (Penn State), Jason Wright (Penn State)

223.11 – Stellar Variability in the M2 and M3Globular ClustersWe present results from an on-going project to understandthe enrichment of the interstellar medium by evolvedmetal-poor stars, particularly while they are on the red andasymptotic giant branches. Our project is targeting globularclusters and nearby galaxies, as these have relatively wellknown global properties such as metallicity, age, anddistance. Here, we present near-infrared observations ofthe globular clusters M2 and M3 in the Milky Way. Theseclusters served as calibration targets for the Galacticpolarization project GPIPS with Mimir on the 1.8m Perkinstelescope. As such, they were observed several times in Hand K bands from 2008 to 2012, which enables us toidentify the long period variables in the clusters,particularly when combined with older data from the2MASS project. Comparing the variability properties of thestars with their locations on the color-magnitude diagramsallows us to estimate the time the stars spend in thesestages of their post-main sequence evolution. We will alsocompare M2 and M3 to our previous results for M5 andM15, which have higher and lower metallicities,respectively.Author(s): Kathleen Kraemer (Boston University), G. Sloan (CornellUniversity), Dan Clemens (Boston University), E. Lagadec (Observatoire dela Cote d'Azur), D. Barry (Cornell University), C. Goes (Cornell University)

223.12 – The Motif of Globular Clusters andLow Mass X-ray Binaries in Ellipticals: a Taleof Three GalaxiesI will discuss significant inhomogeneities in the projectedtwo-dimensional spatial distributions of Globular Clustersand Low Mass X-Ray Binaries observed in three ellipticalgalaxies with extensive spatial coverage in the optical andX-ray: NGC4261, NGC4649 and NGC4278. The spatialstructures in the distributions of GCs and LMXBs have beendetected with a new method based on the K-NearestNeighbor density estimator of Dressler (1980),complemented by MonteCarlo simulations to establish thestatistical significance of the results. I will present thespatial structures as a function of the color and luminosityof the GCs, and will compare their shape and significancewith the spatial distribution of field LMXBs. I will thenexamine the nature of these structures in the context of theevolution history of the host galaxies.Author(s): Raffaele D'Abrusco (SAO), Giuseppina Fabbiano (SAO),Stefano Mineo (SAO), Jay Strader (Michigan State University), TassosFragos (SAO), Dong-Woo Kim (SAO), Bin Luo (Pennsylvania StateUniversity), Andreas Zezas (SAO)

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223.13 – Exploring the Formation ofGalaxies through Metallicities of GlobularClustersGlobular clusters (GCs) are among the oldest stellar objectsin the universe. They have long served the role of providingconstraints on many aspects of galaxy evolution theory.Bimodal color distribution of GC systems in many luminousearly-type galaxies is an observationally establishedphenomenon and has been interpreted as evidence of twoGC subgroups with different metallicities. In this study, weuse spectroscopic data on the GC systems of two giantgalaxies, M31 (the Andromeda) and M87 (NGC 4486), toinvestigate the GC bimodality and the underlyingmetallicity distributions. Recent high signal-to-ratiospectroscopic data on M31 GCs revealed a clear bimodalityin absorption-line index distributions of old GCs. Given thatspectroscopy provides a more robust probe into stellarpopulation than photometry, the reported spectral lineindex bimodality may indicate the presence of two distinctGC populations. However, here we show that thespectroscopic dichotomy of M31 GCs is due to the nonlinearnature of metallicity-to-index conversion and therefore onedoes not need two separate GC subsystems. We considerthis as an analogy to the recent interpretation in whichmetallicity-color nonlinearity is the prime cause forobserved GC color bimodality. We present spectra of ~130old globular clusters (GCs) associated with the Virgo giantelliptical galaxy M87, obtained with the Multi-ObjectSpectrography (MOS) mode of Faint Object Camera andSpectrograph (FOCAS) on the Subaru telescope. Thefundamental properties of globular clusters such as age,metallicity and elemental abundance ratio are investigatedby comparing with a set of Simple Stellar Population (SSP)models. M87 GCs with reliable metallicity measurementsexhibit significant inflection along the color-metallicityrelations, through which observed color bimodality is

reproduced using a broad, unimodal metallicity distribution.Our findings lend further support to this new interpretationof the GC color bimodality, which could change much of thecurrent thought on the formation of GC systems and theirhost galaxies.Author(s): Sooyoung Kim (Yonsei University), Suk-Jin Yoon (YonseiUniversity), Chul Chung (Yonsei University), Nelson Caldwell (Center forAstrophysics), Ricardo Schiavon (Liverpool John Moores University), YongBeom Kang (Chungnam National University), Soo-Chang Rey (ChungnamNational University), Young-Wook Lee (Yonsei University), Naoyuki Tamura(Kavli Institute for the Physics and Mathematics of the Universe), S. TonySohn (Space Telescope Science Institute), Nobuo Arimoto (NationalAstronomical Observatory of Japan), Tadayuki Kodama (NationalAstronomical Observatory of Japan), Yoshihiko Yamada (NationalAstronomical Observatory of Japan)

223.14 – Hierarchical Star Formation inLEGUS GalaxiesStar formation generally follows a hierarchical distributionin galaxies from kpc scales in giant star complexes down tosub-pc scales in embedded clusters. This hierarchycorresponds to a power law distribution function for thenumber of star forming regions as a function of size orluminosity. Using the Legacy ExtraGalactic UltravioletSurvey (LEGUS), we examine six galaxies, NGC 1566, NGC1705, NGC 2500, NGC 5253, NGC 5477, and IC 4247, whichspan types from grand design and flocculent spirals toirregulars and starburst irregulars. Power law size andluminosity distributions were measured from Gaussian-blurred images in the NUV and UV using SExtractor. Slopesranged from -1 to -1.8, with the steepest slopescorresponding to the starburst galaxies. The slopes did notvary from the NUV to the UV. The fraction of light containedwithin the largest scales ranged from 85 to 95 percent,independent of galaxy type. We acknowledge support fromgrant HST-GO-13364.Author(s): Debra Elmegreen (Vassar College), Bruce Elmegreen (IBMT.J. Watson Res. Ctr.)

Contributing teams: LEGUS

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201 – On the Shoulders of Giants: Planets Beyond the Reach of Kepler I: WhatWe Know Today and What We Would Like to LearnMeeting-in-a-Meeting – America Ballroom North/Central – 03 Jun 2014 10:00 AM to 11:30 AM

What kind of planets lie at orbit radii of 1-2 AU - beyond the reach of Kepler? In the last two decades we haveexplored a large sample of RV-detected and transit-detected planets, discovered distant planets with microlensingand several hot young planets at large radii using direct imaging, as well as the debris disks that provide clues toformation and evolution. In these 4 sessions, we explore the near future, and how we can expect to learn muchmore about the demographics and properties of cold outer planets. WFIRST-AFTA will open up this area, with amicrolensing survey to probe the population of long-orbit planets, and coronagraphy to take images and spectraof large planets in orbits at a few AU. Session I covers an introduction to this Meeting-in-Meeting, and presents thecurrent state of theoretical understanding of planets in long orbits - beyond the reach of Kepler.

Chair(s):Stephen Unwin (JPL)

201.01 – Planets Beyond the Reach ofKepler - IntroductionWhat kind of planets lie at orbit radii of 1-2 AU - beyond thereach of Kepler? In the last two decades we have explored asample of RV-detected planets, discovered distant planetswith microlensing, and several hot young planets at largeradii have been detected by direct imaging, as well as thedebris disks that provide clues to formation and evolution.In these 4 sessions, we explore the near future, and how wecan expect to learn much more about the demographicsand properties of cold outer planets. AFTA-WFIRST will openup this area, with a microlensing survey to probe thepopulation of long-orbit planets, and coronagraphy to takeimages and spectra of large planets in orbits at a few AU.Author(s): Stephen Unwin (JPL)

201.02 – Studying Extrasolar Planets withWFIRSTThe WFIRST mission will be a powerful tool for studyingextrasolar planets. Through observations of gravitationalmicrolensing, the mission will probe the demographics ofextrasolar planetary systems. Its coronagraph will enableimaging and spectroscopic study of nearby planets. It willalso be able to complement GAIA's astrometricmeasurements of masses and orbits of nearby planets.Author(s): David Spergel (Princeton Univ. Obs.)

201.03 – Theory of giant planetatmospheres and spectraGiant exoplanet atmospheres have now been studied bytransit spectroscopy, spectroscopy and photometry atsecondary eclipse, photometric light curves as a function oforbital phase, very high-resolution spectroscopic velocitymeasurements, and high-contrast imaging. Moreover, thereis a correspondence between brown dwarf and giant planetatmospheres and spectra that has been profitably exploitedfor many years to better understand exoplanets. In thispresentation, I endeavor to review the informationextracted by these techniques about close-in giantexoplanet compositions and temperatures. Then, I willsummarize the expected character of the spectra, lightcurves, and polarizations of the objects soon to be studiedusing high-contrast imaging by GPI, SPHERE, WFIRST-AFTA,and Subaru/HiCIAO as a function of mass, age, Keplerianelements, and birth properties (such as entropy). The goalwill be to frame the theoretical discussion concerning whatphysical information can be gleaned in the next yearsabout giant planet atmospheres by direct (or almost direct)imaging and characterization campaigns, and their role asstepping stones to the even more numerous sub-Neptunes,super-Earths, and Earths.Author(s): Adam Burrows (Princeton University)

201.04 – Observed & Predicted Debris DisksStructures Beyond the Reach of KeplerOver the last several years our theoretical understanding ofdebris disks has evolved significantly. A number of newcomputational advances, in the realms of disk modelingand data analysis, have deepened our knowledge ofstructures in debris disks. More than ever, we are acutelyaware of the many sources of structures--be theygravitational perturbations by planets, other externalperturbations, or more subtle non-perturbative sources. Atthe same time, new observatories, instruments, andobservation strategies have provided a rich data set fordebris disk theorists to test and constrain their models. Iwill discuss our current understanding of structures indebris disks. I will show the wide array of structures thatplanets can dynamically sculpt and comment on howimaging of these structures with future missions mayconstrain the underlying planetary system. I will alsopresent a cautionary tale of interpreting debris diskstructures as planetary perturbations, show how ourappreciation of alternative sources of structures has grown,and present new methods for disentangling true densitystructures from projection and scattering effects.Author(s): Christopher Stark (NASA Goddard Space Flight Center)

201.05 – Theoretical Albedo Spectra ofExoplanet Direct Imaging TargetsSpace-based coronagraphic telescopes currently understudy would enable direct imaging of scattered light fromgiant exoplanets in orbits beyond 1 AU from their hoststars. Considering the known radial-velocity planets alone,directly imaged planets will encompass a broad range ofatmospheric properties, including a number of possiblecloud species. Here we present theoretical albedo spectra(0.35 to 1 micron) for the most favorable targets forspaced-based coronagraph observations (good angularresolution and contrast) from the current population ofknown radial-velocity planets. We consider a range ofinternal temperatures and atmospheric metallicities asconstrained by the system ages and planetary minimummasses. Additionally, we construct a grid of theoreticalJupiter and Neptune-like exoplanets around a variety ofhost stars at distances of 1, 3, and 5 AU. From this grid, weidentify spectral and photometric signatures associatedwith planetary gravity, cloudiness, and composition thatcan used to select promising new targets as they arediscovered. This work will help to guide the developmentand initial interpretation of a range of direct imagingexoplanet studies that will shed new light on importantphysical processes underlying giant planet formation andevolution.Author(s): Nikole Lewis (MIT), Mark Marley (NASA/Ames), JonathanFortney (UCSC)

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202 – Solar Surface and Interior IMeeting-in-a-Meeting – America Ballroom South – 03 Jun 2014 10:00 AM to 11:30 AMChair(s):Rudolf Komm (National Solar Obs.)

202.01 – A Helioseismic Survey of EmergingActive Regions Using HMI-SDO DataA survey of the subsurface properties of approximately 100emerging active regions, determined from the applicationof helioseismic holography to Dopplergrams obtained withthe HMI instrument onboard the Solar DynamicsObservatory, is being carried out. The goal of this researchis to use helioseismology and numerical simulations toidentify and understand possible signatures, in the form ofacoustic travel time shifts, due to rising magnetic fluxconcentrations prior to their emergence at the solarphotosphere. The status of the project and current resultswill be discussed. We make use of ensemble averages oftravel-time shift measurements as proxies for near-surfacedepth-integrated wave-speed changes and flows. The latterinclude horizontal components of the flows as well as theirhorizontal divergence and the vertical component of theflow vorticity. A control sample of a similar number ofquiet-Sun regions is used for comparison and for identifyingpotential systematic effects. Preliminary results confirmprevious suggestions (obtained from a prior survey usingGONG data) that emergence sites are associated withconverging photospheric flows, such as the boundaries ofsupergranulation. This work is supported by the NASAHeliophysics Supporting Research program throughcontract NNH12CF23C.Author(s): Douglas Braun (NorthWest Research Associates, Inc.),Hannah Schunker (Max-Planck-Institut für Sonnensystemforschung), AaronBirch (Max-Planck-Institut für Sonnensystemforschung)

202.02 – Using SDO/HMI Observations toDetect Pre-emergence Signatures of LargeActive RegionsIt was shown that large active regions can be detected byhelioseismology in the deep convection zone before theybecome visible in the photosphere. The detection method isbased on computations of cross-covariances betweenoscillation signals observed at pairs of locations on thesolar surface. We present in this study the results of athorough helioseismic investigation of large emergingactive regions observed with SDO/HMI. For each one ofthese regions, we monitor the subsurface acousticperturbations at various depths up to about 75 Mm and forseveral days before the emergence of magnetic field in thephotosphere. The same set of measurements is alsoapplied to quiet regions to obtain estimates of the noiselevel and evaluate the statistical significance of theperturbations measured in emerging-flux regions. We showexamples of positive detection with the correspondingconfidence levels, and we discuss perspectives of using thismethod with near real-time data from SDO/HMI to forecastthe emergence of large active regions.Author(s): Stathis Ilonidis (Stanford University), Junwei Zhao(Stanford University)

202.03 – Comparing helioseismicmeasurements over a numericallysimulated sunspot with ray-tracing methodWe perform helioseismic analysis over numericallysimulated data by Rempel et al. (2009 Science), andcompare the measured acoustic travel-time shifts with theexpected values. We calculate the synthetic acoustic traveltime using ray-tracing method on the sunspot model withall necessary field properties of the subsurface, includingsunspot geometry, sound-speed perturbation, magneticfield,and flow velocity. Comparing with travel times in thequiet region, each of these properties contributes to a -80,+40,-20, +/-5 sec time shift, respectively, for a distance of~20Mm. The helioseismic measurements from thesimulated data using the same sunspot model arecomparable to the measurements from observed sunspots.There is a clear travel-time asymmetry in waves travelinginto and out from the sunspot, and this cannot be solelydue to the flow velocity according to the ray-tracingmethod. We discuss possibilities of how to explain thistravel-time asymmetry.Author(s): Ruizhu Chen (Stanford Univ.), Junwei Zhao (Stanford Univ.)

202.04 – Numerical simulations of sunspotdecay: On the role of a penumbra andsubsurface field structureWe present high-resolution simulations of decayingsunspots that cover a time span of up to 100 hours. Thesimulations reach 18Mm deep into the convection zone anduse open boundaries that do not maintain the initial fieldstructure against decay driven by convective motions. Wediscuss three experiments: A sunspot simulation withpenumbra, a "naked-spot" simulation in which we removedthe penumbra after 20 hours, and a sunspot simulationwith penumbra, but a less coherent subsurface fieldstructure. In all three simulations we study the decayprocess and large-scale flows in proximity of the spots.Over the time span covered by the simulation the spot withpenumbra is almost stationary with regard to the total fluxcontent, but shows a steady decay of the flux present inthe umbra area at a rate comparable to the "naked-spot"experiment. A less coherent sub-surface magnetic fieldstructure leads within 12-24 hours to a less coherentsurface appearance, i.e. details of the subsurface structuredo not remain hidden from the photosphere. In all threeexperiments the dominant subsurface flow patterns areoutflows.Author(s): Matthias Rempel (NCAR)

Contributing teams: NASA SDO-Science Center

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202.05 – North-South Flow Asymmetries inthe Rising Phase of Solar Cycle 24Sub-surface solar flows can be inferred using acousticwaves measured at the solar surface, and making thesemeasurements is one of the principal applications ofhelioseismology. Four years of high-duty-cycle,high-cadence, high-resolution data from the Helioseismicand Magnetic Imager (HMI) on the Solar DynamicsObservatory (SDO) provides an ideal data set to which toapply local helioseismic techniques and study spatiallyresolved structures in sub-surface flows. In this work, weattempt to characterize the differences in near-surfaceflows between the north and south solar hemispheres usingdata from HMI's ring-diagram analysis pipeline. It iswell-known that solar surface activity in the North andSouth hemispheres is out of phase, and it is of particularinterest to determine how deep this asymmetry penetrates.Author(s): Charles Baldner (Stanford University), Richard Bogart(Stanford University)

202.06 – Influence of Magnetic and ThermalEffects on Helioseismic Travel-time Shifts inSunspot ModelsSunspots are one of the most prominent manifestations ofsolar magnetic activity and have been studied using localhelioseismology for decades. Recent modeling andobservational studies indicate that the interpretation oftravel-time shifts is still subject to uncertainties regardingthe physical causes of the wave perturbations. Numericalwave propagation has proved useful in addressing thisproblem. In this work, we have analyzed travel-time shiftsobtained from three dimensional numerical simulations ofwave propagation in a magnetohydrostatic sunspot-likeatmosphere. In particular, we isolate the individual effectsof the magnetic field and thermal perturbations on themeasurements by means of simulations where only onekind of perturbation (magnetic or thermal) is included. Theresulting travel-time shift maps, obtained by applyinghelioseismic holography to the photospheric Dopplersignals in the simulated domain, will be compared anddiscussed. We plan to make the artificial data available tothe community for the development and validation of otherhelioseismic methods. This work is supported by the NASASDO Science Center program (through contractNNH09CE41C) and by the NASA Living With a Star Program(through grant NNX14AD42G).Author(s): Tobias Felipe (NorthWest Research Associates), DouglasBraun (NorthWest Research Associates), Ashley Crouch (NorthWestResearch Associates), Aaron Birch (Max-Planck-Institut furSonnensystemforschung)

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203 – History of Solar PhysicsMeeting-in-a-Meeting – Staffordshire – 03 Jun 2014 10:00 AM to 11:30 AMChair(s):Jay Pasachoff (Williams College)

203.01 – The Discovery of the Solar5-minute Oscillations and theSupergranulationThe summer of 1960 marked the discovery, from the Mt.Wilson 60-foot solar tower telescope, of both the solar5-minute oscillation and the supergranulation. We reviewthe history of how, starting in 1955, Robert Leighton atCaltech carried out studies of the sun at high resolutionfrom the Mt. Wilson 60-foot solar tower telescope. In 1958he developed a method to map the spatial distribution ofsolar magnetic fields by photographically subtracting pairsof spectroheliograph images differing only in the sign oftheir Zeeman-effect sensitivity to longitudinal magneticfields, and showed for the first time that photosphericmagnetic fields trace out the heating of the overlyingchromosphere as revealed by the pattern of the Ca IIemission network. Leighton then developed a variation ofthe technique to measure velocity fields and their spatialand temporal variation, and in the summer of 1960 he andhis students made a series of discoveries that changed theface of solar physics. One of these was the discovery thatthe velocity field of the sun exhibits a very strong quasi-periodic vertical oscillation with a period of about 5minutes; this discovery represents the dawn ofhelioseismology, which over the past 50 years has grown toembrace research lines in solar and stellar astrophysicsthat were unimaginable at the time. A parallel discoverymade by Leighton and his students during that samesummer was the "large cells", later to be termed thesupergranulation, which show a complex pattern of flowfields, evidently produced by large-scale convectivemotions that are still not well-understood, but which createthe magnetic network and hence the pattern of heating inthe overlying chromosphere.Author(s): Robert Noyes (Center for Astrophysics)

203.02 – Origin of the Wang-Sheeley-ArgeSolar Wind ModelA correlation between solar wind speed at Earth and theamount of field line expansion in the corona was verified in1989 using 22 years of solar and interplanetaryobservations. This talk will trace the history of thisdiscovery from its birth 15 years earlier in the Skylab era toits current use as a space weather forecasting technique.This research was supported by NASA and ONR.Author(s): Neil Sheeley (Naval Research Laboratory)

203.03 – Lockheed Solar Observatory andthe Discovery of Moreton-Ramsey WavesMoreton Waves are high-speed disturbances seen travelingaway from large solar flares in H-alpha movies of the solarchromosphere. They were discovered by the observer HarryRamsey in the late 1950s, and then published andpublicized by the director Gail Moreton, both of theLockheed Solar Observatory in the Hollywood Hills ofSouthern California. These efforts established the scientificreputation and secured continuing funding of theobservatory, whose present-day successor is the LockheedMartin Solar and Astrophysics Lab in Palo Alto. Moretonwaves are rare, and there was limited interest in them untilthe EIT instrument on SOHO began seeing large numbers ofsimilar waves in the corona in the late 1990s. The exactrelation between the two observations is still a researchtopic today. This talk will describe some of the history of theobservatory and the discovery and early interpretation ofthe waves.Author(s): Theodore Tarbell (Lockheed Martin Solar andAstrophysics Laboratory)

203.04 – On the Naming and Dscovery ofthe Solar ChromosphereThe chromosphere was discovered by Lockyer and Janssenin 1868, and named by Lockyer. It is often stated that hismotivation for associating this region of the solaratmosphere with "color" was because of its bright redappearance at eclipses due to the predominance ofH-alpha. However, Lockyer had never seen a total solareclipse at the time he gave the name and does not appearto have provided this justification himself. It is more likelythat the "color" refers to the plethora of different coloredemission lines he saw and identified with his spectrograph.I also discuss the Padre Angelo Secchi's observation of the1860 eclipse in Spain, His accurate description of thechromosphere as a complete, theretofore unseen layerenveloping the Sun predates Lockyer and Janssen by eightyears.Author(s): Kevin Reardon (National Solar Observatory)

203.05 – Constructing 'Black Sun': theDocumentary Film of the 2012 Eclipses2012 offered an opportunity that was not to be missed: twosolar eclipses. Drs Alphonse Sterling and Hakeem Oluseyibegan doing collaborative research during total solareclipses in 2006 in Ghana. Since then they have continuedto do eclipse observation when funds and whetherpermitted. As a filmmaker, the opportunity to film Sterlingand Oluseyi during the 2012 eclipses in Tokyo and Cairnsfulfilled the goal of showing the excitement oftime-sensitive research, the lives of astrophysicists, anddiversity within the astronomy community. As anastrophysicist who did not specialize in solar astrophysics,it was an opportunity for me both to learn and to solidify forthe audience what we know about the sun and theimportance of eclipse observation. Clips of the film will beincluded.Author(s): Jarita Holbrook (University of the Western Cape)

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203.06 – Howard Russell Butler's OilPaintings of Solar Eclipses and ProminencesHoward Russell Butler (1856-1934) was invited to join theUS Naval Observatory expedition to the total solar eclipseof 1918 because of his ability to paint astronomicalphenomena based on quickly-made notes about spatial andcolor details. His giant triptych of the total eclipses of 1918,1923, and 1925 was proposed for a never-builtastronomical center at the American Museum of NaturalHistory and wound up at their Hayden Planetarium when itwas constructed in the mid-1930s. Half-size versions areinstalled at the Fels Planetarium at the Franklin Institute inPhiladelphia and at the Firestone Library of PrincetonUniversity, whose newly conserved canvases were recentlyhung; the Buffalo Museum of Science has another half-sizeversion in storage. We discuss not only the eclipse triptychsbut also the series of large oil paintings he made of solarprominences (in storage at the American Museum ofNatural History) and of his 1932-eclipse and other relevantworks. JMP was supported for this work in part by DivisionIII Discretionary Funds and the Brandi Fund of WilliamsCollege. His current eclipse research is supported by grantsAGS-1047726 from the Solar Research Program of the

Atmospheric and Geospace Sciences Division of NSF and9327-13 from the Committee for Research and Explorationof the National Geographic Society.Author(s): Jay Pasachoff (Williams College), Roberta J. M. Olson(New-York Historical Society)

203.07 – Exceptional Portable Sundials atHarvardThe Collection of Historical Scientific Instruments atHarvard University has the largest assemblage of sundialsin North America. The dials date from the 16th to the 19thcenturies, and most are designed to be carried in one’spocket or put on a window sill. They take advantage of thesun’s changing altitude, azimuth, hour angle, or acombination of the foregoing in order to find the time. Manyare also usable at a wide range of latitudes, and thereforeare suitable tools for travelers. Fashioned of wood, paper,ivory, brass, and silver, the sundials combine mathematicalprojections of the sun’s apparent motion with artistry,fashion, and exquisite craftsmanship. This paper willexplore the wide variety of sundials and what they tell usabout the people who made and used them.Author(s): Sara Schechner (Harvard Univ.)

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204 – Black Holes, Pulsars, and Neutron StarsOral Session – St. George AB – 03 Jun 2014 10:00 AM to 11:30 AMChair(s):Jonathan Grindlay (Harvard-Smithsonian, CfA)

204.01 – General relativistic simulations ofoptically thick accretion disks.Only recently numerical codes solving accretion on blackholes in full general relativity with approximated radiativetransfer have been developed. Such tools make studies ofthin and super-critical, optically thick accretion diskspossible. I will report on recent developments in this fieldputting most attention to hyper-accreting disks.Author(s): Aleksander Sadowski (Harvard-Smithsonian Center forAstrophysics), Ramesh Narayan (Harvard-Smithsonian Center forAstrophysics), Jonathan McKinney (University of Maryland), AlexanderTchekhovskoy (University of California)

204.02 – Particle Acceleration byRelativistic Frame Dragging of aMagnetised Black HoleBlack holes are considered to be a likely agent ofacceleration of particles. Various processes have beenproposed, however, the exact mechanism is still to beidentified. It is conceivable that different mechanisms canoperate, depending on parameters of the black hole (spin)and the environment to which the black hole is embedded(magnetic fields and plasma). We demonstrate thatlarge-scale oblique magnetic field near a rotating (Kerr)black hole acts as an origin of magnetic layers, where thefield direction changes abruptly (Karas, Kopacek, &Kunneriath 2012, 2013). Magnetic null points can developnear the ergosphere boundary by purely geometricaleffects of the strong gravitational field and the frame-dragging mechanism. In consequence, particles can beaccelerated efficiently by the gravito-magnetically inducedelectric component. The situation we discuss is relevant forstarving nuclei of some galaxies which exhibit episodicaccretion events, such as Sagittarius A* supermassive blackhole surrounded by the large-scale structure of magneticfilaments. By the mass-scaling relation, the same process isexpected to operate also near a stellar-mass black holeorbiting in a close binary system with a stronglymagnetised neutron star.Author(s): Vladimir Karas (Astronomical Institute, Academy ofSciences), Ondrej Kopacek (Astronomical Institute, Academy of Sciences),Devaky Kunneriath (Astronomical Institute, Academy of Sciences)

204.03 – A New Physical Model for Pulsarsas Gravitational Shielding and OscillatingNeutron StarsPulsars are fast rotating neutron stars that synchronouslyemit periodic Dirac delta shape pulses of radio-frequencyradiation and Lorentzian shape oscillations of X-rays. Theacceleration of particles near the magnetic poles, whichderivate from the rotating axis produces coherent beams ofradio emissions that are viewed as pulses of radiationwhenever the magnetic poles sweep the viewers. However,the conventional lighthouse model of pulsars is onlyconceptual. The physical mechanism through whichparticles are accelerated to produce coherent beams ofradio emissions is still poorly understood. The process forperiodically oscillating X-rays to emit from hot spots at theinner edge of accretion disks of pulsars is also remained asan unsolved mystery. Recently, a new physical model ofpulsars is proposed by the author to quantitatively interpretthe emission characteristics of pulsars, in accordance withhis well-developed five-dimensional fully covariantKaluza-Klein gravitational shielding theory and the physicsof thermal and accelerating charged particle radiation. Theresults indicate that with the significant gravitationalshielding by scalar field a neutron star nonlinearly oscillatesand produces synchronous periodically Dirac delta shapepulse-like radio-frequency radiation (emitted by theoscillating or accelerating charged particles) as well asperiodically Lorentzian shape oscillating X-rays (as thethermal radiation of neutron stars that temperature variesdue to the oscillation). This physical model of pulsars asgravitational shielding and oscillating neutron starsbroadens our understanding of neutron stars and developsan innovative mechanism to disclose the mystery ofpulsars. In this presentation, I will show the results obtainedfrom the quantitative studies of this new physical model ofpulsars for the oscillations of neutron stars and the powersof radio pulse-like emissions and oscillating X-rays.Author(s): Tianxi Zhang (Alabama A&M University)

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204.04 – General RelativisticMagnetohydrodynamic Simulations ofBlandford-Znajek Jets and the MembraneParadigmRecently it has been observed that the scaling of jet powerwith black hole spin in galactic X-ray binaries is consistentwith the predictions of the Blandford-Znajek (BZ) jet model.These observations motivate us to revisit the BZ modelusing general relativistic magnetohydrodynamicsimulations of magnetized jets from accreting (h/r ~ 0.3),spinning (0 < a_* < 0.98) black holes. We have three mainresults. First, we quantify the discrepancies between the BZjet power and our simulations: assuming maximumefficiency and uniform fields on the horizon leads to a~10% overestimate of jet power, while ignoring theaccretion disk leads to a further ~50% overestimate.Simply reducing the standard BZ jet power prediction by60% gives a good fit to our simulation data. Our secondresult is to show that the membrane formulation of the BZmodel correctly describes the physics underlying simulatedjets: torques, dissipation, and electromagnetic fields on thehorizon. This provides intuitive yet rigorous pictures for theblack hole energy extraction process. Third, we computethe effective resistance of the load region and show thatthe load and the black hole achieve near perfectimpedance matching. Taken together, these resultsincrease our confidence in the BZ model as the correctdescription of jets observed from astrophysical black holes.Author(s): Robert Penna (MIT), Ramesh Narayan (Harvard), AleksanderSadowski (Harvard)

204.05 – A Link Between X-ray EmissionLines and Radio Jets in 4U 1630-47?Recently, Díaz Trigo et al. reported an XMM-Newtondetection of relativistically Doppler-shifted emission linesassociated with steep-spectrum radio emission in thestellar-mass black hole candidate 4U 1630-47 during its2012 outburst. They interpreted these lines as indicative ofa baryonic jet launched by the accretion disk. We present asearch for the same lines earlier in the same outburst usinghigh-resolution X-ray spectra from the Chandra HETGS.While our observations (eight months prior to theXMM-Newton campaign) also coincide with detections ofsteep spectrum radio emission by the Australia TelescopeCompact Array, we find a strong disk wind but no evidencefor any relativistic X-ray emission lines. Indeed, despite ?5×brighter radio emission, our Chandra spectra allow us toplace an upper limit on the flux in the blueshifted Fe XXVIline that is ?20× weaker than the line observed by DíazTrigo et al. Thus we can conclusively say that radioemission is not universally associated with relativisticallyDoppler-shifted emission lines in 4U 1630-47. We exploreseveral scenarios that could explain our differing results,including variations in the geometry of the jet or amass-loading process or jet baryon content that evolveswith the accretion state of the black hole. We also considerthe possibility that the radio emission arises in aninteraction between a jet and the nearby ISM, in which casethe X-ray emission lines might be unrelated to the radioemission.Author(s): Joseph Neilsen (MIT Kavli Institute), Mickaël Coriat(University of Cape Town), Rob Fender (Oxford University), Julia Lee(Harvard-Smithsonian Center for Astrophysics), Gabriele Ponti (Max PlanckInstitute fur Extraterrestriche Physik), A. Tzioumis (Australia TelescopeNational Facility), Phillip Edwards (Australia Telescope National Facility),Jess Broderick (University of Southampton)

204.06 – Polarimetry with the Event HorizonTelescopeThe Event Horizon Telescope (EHT) is an effort to developmillimeter and submillimeter VLBI to image nearby blackholes at resolutions comparable to their event horizons.Past work with the EHT has measured compact emission onsuch scales for Sgr A* and M87, and has also measuredsub-parsec structure in more distant quasars. Polarimetrywith the EHT enables a powerful extension of this work,mapping magnetic field structures via the highly polarizedsynchrotron emission. Polarization is also an excellentprobe of rapid variability, especially for Sgr A*, and canconvey rich astrometric information even with incompleteimaging. We report on results from our 2013 campaign,which demonstrate a sharp increase in the linearpolarization fraction and variability with increasingbaseline, and we demonstrate that current EHT data canpotentially achieve microarcsecond relative astrometry offlaring regions on timescales of minutes.Author(s): Michael Johnson (Harvard-Smithsonian Center forAstrophysics), Sheperd Doeleman (Massachusetts Institute ofTechnology), Vincent Fish (Massachusetts Institute of Technology), RichardPlambeck (University of California, Berkeley), Daniel Marrone (University ofArizona), Michael Kosowsky (Brandeis University), John Wardle (BrandeisUniversity), Rusen Lu (Massachusetts Institute of Technology)

Contributing teams: EHT Collaboration

204.07 – A Survey for CosmologicalMillisecond Radio Transients with the VeryLarge ArraySingle-dish pulsar surveys have revealed a new populationof millisecond radio transients that seem to originate atcosmological distances. If indeed cosmological, these "fastradio bursts" (FRBs) are orders of magnitude brighter thanany known millisecond radio transient, yet about asfrequent as core-collapse supernovae. That would makethem powerful probes of the intergalactic medium andpotentially tracers of exotic new physics, such as doubleneutron star systems that are expected to produce the firstgravitational wave detections. We will present the latestresults from an ongoing large survey for FRBs with the VeryLarge Array (VLA). Interferometric detection will definitivelyshow these events are astrophysical and, if extragalactic,will uniquely associate FRBs with host galaxies to measurethe baryon density of the IGM in an entirely new way. Thiscampaign uses a new observing mode that produces 1terabyte per hour and can image the sky with 5 mscadence, making the VLA into a powerful platform forwide-field fast transient surveys.Author(s): Casey Law (UC Berkeley), Geoffrey Bower (UC Berkeley),Sarah Burke-Spolaor (Caltech), Michael Rupen (NRAO), Bryan Butler(NRAO), Scott VanderWiel (LANL), Joseph Lazio (JPL), Earl Lawrence (LANL),Andrew Siemion (UC Berkeley), Chris Mattmann (JPL)

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204.08 – Probing Relics of Galaxy Formationwith Cosmic Clocks: Pulsars in GlobularClustersGlobular clusters are relics of galactic formation. There aremore than a hundred of these star clusters in our ownGalaxy. These spherical collection of stars are typicallymade up of very old stellar populations and therefore holdclues about the very early stages of galaxy evolution.Hence, understanding these clusters is critically importantin solving the galactic jigsaw puzzle. It typically takes very

long observational efforts to analyze thousands ofindividual stars in order to infer important kinematicparameters for each globular cluster. Here we show ananalytically tractable method that enables us to probethese globular cluster properties with only a handful ofpulsars. Additionally, probing the kinematics of globularclusters through a distinct population of compact stars hasother advantages. It enables us to probe the very centersof these clusters that may harbor massive black holes.Author(s): Bülent Kiziltan (Harvard-Smithsonian Center forAstrophysics)

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205 – Bridging Laboratory & Astrophysics: Dust & IcesMeeting-in-a-Meeting – St. George CD – 03 Jun 2014 10:00 AM to 11:30 AM

Laboratory astrophysics is the Rosetta Stone that enables astronomers to understand and interpret the cosmos.This session will focus on the interplay between astrophysics with theoretical and experimental studies into theunderlying dust and ice processes, which drive our Universe.

Chair(s):Gianfranco Vidali (Syracuse Univ.)Organizer(s):Farid Salama (NASA Ames Research Center)

205.01 – Some Open Questions in thePhysics of Interstellar DustOur efforts to understand interstellar dust proceed by tryingto develop models that are consistent with the laws ofphysics as well as with the many observational constraintsprovided by astronomical observations, the meteoriticrecord, and observations of interstellar dust grains enteringthe solar system today. I will review some open questions inphysics and surface chemistry that are important forcurrent modeling of dust. Nature has provided us withhundreds of spectroscopic clues -- the diffuse interstellarbands -- and it is an embarrasment that we haven't yetbeen able to decipher them. Interstellar grains contain iron,which could be in ferromagnetic or ferrimagnetic materials.If so, does magnetic dissipation contribute significantly toemission from dust at microwave and submm frequencies?This can be addressed in the laboratory. We do know thatinterstellar grains are not spherical, but we don't knowwhether they are compact, or whether they are haveextended "fluffy" structures. To find out, we will have tocompare observed optical properties of interstellar dustwith theoretical models. How can we calculate the opticalproperties of fluffy grains at wavelengths ranging fromX-rays to far-infrared? Theoretical methods will bedescribed. It seems very likely that interstellar grains areoften destroyed in the ISM; if so, then the observedabundance of grains requires that new grain material beformed in interstellar space. How can grain materials"grow" in the ISM? In particular, is it possible to growamorphous silicates in cold interstellar clouds? What aboutcarbonaceous material, in particular the nanoparticles thatare thought to be responsible for the strong "PAH" emissionbands? The possibilities and limitations of laboratorystudies will be discussed.Author(s): Bruce Draine (Princeton University)

205.02 – Formation of Molecules on CosmicDust Grains:From H2 to AstrobiologyFrontiersIf the role of dust grains in the formation of molecules inthe ISM is now well accepted (as suggested almost 50years ago) numerous questions remain yet unresolveddespite serious experimental and theoretical efforts. This isthe case for H2 (after ~20 years research) and morerecently for larger molecules. For the latter the topical hotproblem is to find a link between astrophysics andastrobiology in search of the origin of life in the universe,obviously a key question of paramount interest and generalfascination. Both laboratory experiments and theory arenecessary to interpret the wealth of increasingobservational results and their improvements through newinstrumental developments. The aim is to derive from themthe physical and chemical conditions (and/or their dynamicevolution) in the remote regions of the ISM. In thelaboratory a variety of multi-disciplinary experimentalapproaches are used to study the large number ofparameters involved in the catalytic role of dust grains inthe formation process and its different stages. The first stepis to manufacture analogs of a dust grain, using severaltechniques. The most important parameters of a dustsurface (and volume) are its nature and morphology.Carbonaceous or siliceous grains are fabricated, either bareor covered by a variety of ices, which have to bewell-characterized. The second step covers the study of theformation mechanism(s) of molecules on a dust surface.This will be illustrated with two examples: H2 and prebioticmolecules. The main interest in the case of H2 is to learnabout the fate of the energy released (~4.5 eV per H2) inthe formation process, due to its determinant role in starformation. In the case of prebiotic molecules the maininterest is that they can be considered as precursors of theformation of complex organic compounds (like amino acids)which are subsequently at the origin of more complexbiological material. The third and particularly importantstep is to establish a connection and feedback betweenobservations and experimental results. An outlook on thesethree aspects will be presented. New perspectives will alsobe discussed.Author(s): Jean Louis Lemaire (Paris-Meudon Observatory)

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205.03 – Atomic Oxygen Desorption from anAmorphous Silicate SurfaceOxygen is the third most abundant element in space. Howoxygen-containing molecules form in space, and whetherthey form through gas-phase or grain-surface reactions,depends largely on the availability of atomic oxygen ingas-phase versus on surfaces of dust grains. The relativeabundance of O in gas-phase versus on grain surfaces isdetermined by the residence time, or equivalently,desorption energy, of atomic oxygen on grain surfaces.Though important in astrochemical modeling, experimentalinvestigations of atomic oxygen desorption from grainsurfaces are lacking in the literature. In most astrochemicalmodels, the O desorption energy value has been taken tobe 800 K, which is a guessed value without experimentalsupport. Based on this value, the predicted molecularoxygen abundance in space is at least 2 orders ofmagnitude higher than what space observations havefound. This long running discrepancy of molecular oxygenabundance could be resolved if the O desorption energy istwice as the widely used value (Melnick, G., Tolls, V., et al.2012, Astrophys. J., 752, 26). We performed TPD (thermalprogrammed desorption) experiments to study the ozoneformation process via O+O2 on an amorphous silicatesurface that emulates interstellar conditions. A rateequation model was used to characterize the surfacekinetics of both atomic and molecular oxygen. The Odesorption energy was extracted from rate equationsimulations that best fit the TPD data. The value was foundto be 1764±232 K, which agrees with what Melnick et al.proposed. We suggest that the newly found value for the Odesorption energy should be used in astrochemicalmodeling. This work is supported by NSF, Astronomy &Astrophysics Division (Grants No. 0908108 and 1311958),and NASA (Grant No. NNX12AF38G). We thank Dr. J.Brucatoof the Astrophysical Observatory of Arcetri for providing thesamples used in these experiments.Author(s): Jiao He (Syracuse University), Gianfranco Vidali (SyracuseUniversity)

205.04 – Photodesorption of InterstellarIces: a Wavelength-dependent Approach toUnveil Molecular MechanismsIn the cold and dense regions of the interstellar medium,non-thermal desorption of interstellar ices drives theice-to-gas ratio of most molecules. More specifically,non-thermal desorption induced by UV photons has beenproposed as the dominating mechanism responsible for theobservation of cold molecular gas in various star-formingenvironments. In protoplanetary disks mid-planes, forexample, UV photons from the pre-main sequence star canpenetrate deep into the disk, reach the ice region andinduce ice sublimation. In prestellar cores and in the outerparts of protostellar envelopes, it is the Lyman-alpha-dominated UV field generated locally by the interaction ofcosmic rays with H2 that can potentially interact with icemantles and result in observable cold molecular gas. Toconstrain the photodesorption mechanism of interstellarices and predict its efficiency for various UV fields, we havedeveloped a novel wavelength-dependent approach usingthe vacuum UV beamline DESIRS at the French synchrotronfacility SOLEIL. Monochromatic tunable UV light in the 7 -14 eV window is used to irradiate interstellar ice analoguesand the rates at which molecules photodesorb aresimultaneously measured using mass-spectrometry. Thefrequency resolved photodesorption spectra of pure CO andN2 ices show a clear UV-wavelength dependency, directlyscaled to the absorption spectra of the condensedmolecules, which hints for a Desorption Induced byElectronic Transition (DIET) process. The application of thistechnique to isotopically labeled layered ices and binary icemixtures has further revealed that CO and N2 icephotodesorption is an indirect process where it is theelectronic excitation of sub-surface species that leads tothe desorption of surface molecules. The photodesorptionefficiency of a species is thus linked to its molecularenvironment and photodesorption rates are different forpure and mixed ices. This has strong implications forastrochemical modeling and could potentially explain the

CO and N2 (N2H+) abundance profiles in prestellar cores.Author(s): Edith Fayolle (Harvard-Smithsonian Center forAstrophysics), Mathieu Bertin (Université Pierre et Marie Curie), ClaireRomanzin (Université Paris-Sud), Xavier Michaut (Université Pierre et MarieCurie), Laurent Philippe (Université Pierre et Marie Curie), Karin Oberg(Harvard-Smithsonian Center for Astrophysics), Harold Linnartz (LeidenObservatory), Jean-Hugues Fillion (Université Pierre et Marie Curie)

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206 – Evolution of GalaxiesOral Session – Gloucester, 2nd Floor – 03 Jun 2014 10:00 AM to 11:30 AMChair(s):Anna Sajina (Tufts University)

206.01 – Background Sky Obscuration byCluster Galaxies as a Source of SystematicError for Weak LensingLensing magnification and lensing shear measurements ofgalaxy clusters rely on an accurate determination of thedensity of background galaxies behind the cluster. Thedependence is indirect for shear (via photometric redshiftcorrection schemes) but direct for magnification. Both ofthese calculations assume a full view of the backgroundsky, but in fact some fraction of the background sky isobscured by the cluster galaxies themselves. We discussthe size of this effect for several current and upcomingcosmological surveys and forecast its impact on clustermass determinations.Author(s): Melanie Simet (Carnegie Mellon University), RachelMandelbaum (Carnegie Mellon University)

206.02 – Correlation Between StarFormation and Substructure in GalaxyClusters using SDSS and WISEWe investigate the relationship between star formation (SF)and substructure in galaxy clusters. Several past studies ofindividual galaxy clusters have suggested that clustermergers enhance cluster SF, while others find no suchrelationship, and so we aim to explore this relationship witha statistical study of large samples of clusters. We firststudy 107 spectroscopically-identified clusters from SDSS,and find that the SF fraction in multi-component clusters(0.228 +/- 0.007) is higher than that in single-componentclusters (0.175 +/- 0.016) for galaxies with M^0.1_r <-20.5. Furthermore, multi-component clusters show ahigher SF fraction than single-component clusters at almostall clustercentric distances and local densities, and we findweak but marginally significant correlations between SFfraction and the level of cluster substructure. In a furtherinvestigation of this relationship, we study a much largersample of over 600 photometrically-selected clusters usingdata from SDSS and WISE. We again find higher amounts ofSF in less-relaxed clusters, which agrees with our previousfindings. These results could indicate that cluster mergersmay cause weak but significant SF enhancement inclusters, or that unrelaxed clusters exhibit slightly strongerSF due to their less evolved states relative to relaxedclusters.Author(s): Seth Cohen (Dartmouth College), Ryan Hickox (DartmouthCollege), Gary Wegner (Dartmouth College)

206.03 – Chandra and XMM-NewtonObservations of the Bimodal Planck-detected Cluster G345.40-39.34 showingHigh and Low Entropy Subcluster CoresThe recent Sunyaev-Zel'dovich (SZ) surveys (from thePlanck mission, the ground based SPT and ACT) haveprovided complete, nearly mass-limited samples of clustersof galaxies. Through extensive X-ray (Chandra andXMM-Newton) follow-up observations of these SZ clustersamples, one can characterize each cluster in terms of itstotal mass, X-ray luminosity, gas mass, gas temperature,entropy, central cooling time, and morphology. Here, wepresent results of Chandra and XMM-Newton observationsof G345.40-39.34, a Planck detected cluster. We show thatG345.40-39.34 is a nearby (z=0.045) double cluster with itssouthern subcluster presenting an interestingthermodynamical characteristic: low global gastemperature and very high central entropy. Because thesetwo simultaneous conditions are rare, we selected clustersthat exhibit similar properties to compare with G345.Finally, we present discussions of the physical processesthat could lead to this unusual thermodynamic state.Author(s): Felipe Andrade-Santos (Harvard-Smithsonian Center forAstrophysics), Christine Jones (Harvard-Smithsonian Center forAstrophysics)

Contributing teams: Chandra Planck Collaboration

206.04 – Chandra and JVLA observations ofthe HST Frontier ClusterMACSJ0717.5+3745Massive merging clusters are excellent laboratories toinvestigate cluster formation and growth, to explore howthe particles that produce cluster-scale diffuse radioemission are accelerated, and to study the nature of darkmatter. Massive clusters, particularly merging clusters withmultiple superposed subhalos, are also powerful cosmictelescopes, capable of magnifying high-z galaxies, thusproviding a probe of the high-z universe. We presentChandra and JVLA observations of the HST Frontier ClusterMACSJ0717.5+3745. This very disturbed cluster isundergoing multiple merger events resulting in shocks andturbulence. Evidence for shocks is also found from theextended radio synchrotron emission observed with theJVLA. In addition, we find several lensed radio and X-raysources behind the cluster. This result demonstrates thefeasibility of deep radio and X-ray studies through thepower of lensing.Author(s): Reinout Van Weeren (Harvard-Smithsonian Center forAstrophysics), Christine Jones (Harvard-Smithsonian Center forAstrophysics), Felipe Santos (Harvard-Smithsonian Center forAstrophysics), William Forman (Harvard-Smithsonian Center forAstrophysics), Scott Randall (Harvard-Smithsonian Center forAstrophysics), Elke Roediger (Hamburger Sternwarte, Hamburg University),Annalisa Bonafede (Hamburger Sternwarte, Hamburg University), RalphKraft (Harvard-Smithsonian Center for Astrophysics), G. Esra Bulbul(Harvard-Smithsonian Center for Astrophysics)

Contributing teams: Chandra Frontier Cluster Team

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206.05 – A Targeted, Distant Galaxy ClusterSurvey Using Bent, Double-Lobed RadioSourcesWe are conducting a large survey of distant clusters ofgalaxies using bent, double-lobed radio sources as tracers.Bent, double-lobed radio sources are driven by AGN andachieve their morphologies through interaction with thesurrounding gas found in clusters. The lobes can becomeswept back during large-scale cluster mergers that set theintracluster medium in motion, or through more gentlesloshing motions of cluster cores driven by more minorinteractions. These types of radio sources may be found inclusters that are highly disturbed as well as those that arerelatively relaxed. In addition, they are found in clusterswith a large range of masses. By the nature of theirselection, all of the clusters will contain radio-loud activegalaxies, so they are expected to be sites of AGN feedback.Based on low-redshift studies, these types of sources canbe used to identify rich clusters with a success rate of~60% (or ~80% if poor clusters and groups are included).We present our survey of 653 bent-double radio sourceswith optical hosts too faint to appear in the SDSS. Thesample was observed in the infrared with Spitzer, and weestimate it will reveal ~400 distant clusters or proto-clusters in the redshift range z ~ 0.7 -- 3.0. The sample ofbent-doubles contains both quasars and radio galaxiesenabling us to study both radiative and kinetic modefeedback in cluster and group environments at a widerange of redshifts.Author(s): Elizabeth Blanton (Boston Univ.), Rachel Paterno-Mahler(Boston Univ.), Joshua Wing (Harvard-Smithsonian Center forAstrophysics), Matthew Ashby (Harvard-Smithsonian Center forAstrophysics), Mark Brodwin (University of Missouri - Kansas City)

206.06 – Spherical accretion and AGNfeedbackFor a supermassive black hole accreting from a hot, quasi-spherical atmosphere, it is almost inevitable that the fluidapproximation fails inside some point within the Bondiradius, but well outside the black hole event horizon. Withinthe region where the particle mean free paths exceed theradius, the flow must be modeled in terms of the Fokker-Planck equation. In the absence of magnetic fields, it isanalogous to the "loss cone" problem for consumption ofstars by a black hole. The accretion rate is suppressed wellbelow the Bondi accretion rate and a significant powermust be conveyed outward for the flow to proceed. Thissituation is complicated significantly by the presence of amagnetic field, but I will argue that the main outcomes aresimilar. I will also argue that the power emerging from sucha flow, although generally far too little to suppress coolingon large scales, is an important ingredient of the AGNfeedback cycle on scales comparable to the Bondi radius.Author(s): Paul Nulsen (SAO)

206.07 – Are local and high-z (U)LIRGsdifferent? A comparison of morphologicaland kinematic properties of local and high-zIR-luminous galaxiesGalaxy interactions/mergers are known to dominate thepopulation of infrared luminous galaxies in the localuniverse (z<0.3), yet it is unclear if this is still the case athigh-z. To test the relative importance of galaxy interactionin the IR-luminouos galaxies, we have carried out acomparison of optical morphological properties betweenlocal and z~1 (U)LIRGs based on the same sampleselection, morphology classification scheme, and opticalmorphology at similar rest-frame wavelengths. Meanwhile,we quantify the systematics in comparing local and z~1datasets by constructing an artificially redshifted datasetfrom local (U)LIRGs, in which its data quality mimics thez~1 dataset. Based on automatic morphology indicators -Gini and M20, we find that the fraction of interactingsystems are similar between local, redshifted, and (U)LIRGsat z<1. Using detailed visual classifications, we show thatthe merger frequency of (U)LIRGs decreases by ~20% fromlocal to z~1, which is comparable to the loss of mergerfraction due to data degradation (~15%). These analysisdemonstrate that no strong evolution of merger frequenciesin (U)LIRGs at least out to z~1. In parallel, we test therobustness of the merger/disk classification schemedeveloped based on the kinematic properties of galaxies(e.g. kinemetry analysis). Using a subset of GOALS galaxieswith IFU observations, we examine the dependence ofkinematic classifications on the data quality. Since thesegalaxies cover a wide range of interaction sequence, wecan also test if the kinematic classifications are able toaccurately determine the merger/disk nature of interactingsystems at different merger stages.Author(s): Chao-Ling Hung (Institute for Astronomy, University ofHawaii), David Sanders (Institute for Astronomy, University of Hawaii),Caitlin Casey (Department of Physics and Astronomy, University ofCalifornia at Irvine), Michael Koss (Institute for Astronomy, ETH Zurich),Kirsten Larson (Institute for Astronomy, University of Hawaii), Nicholas Lee(Institute for Astronomy, University of Hawaii), Yanxia Li (Institute forAstronomy, University of Hawaii), Kelly Lockhart (Institute for Astronomy,University of Hawaii), Hsin-Yi Shih (Institute for Astronomy, University ofHawaii), Howard Smith (Harvard-Smithsonian Center for Astrophysics)

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206.08 – Massive galaxies at z~1-6 from theSpitzer-SERVS plus VISTA-VIDEO surveysWe exploit the uniqueness of the Spitzer RepresentativeVolume Survey (SERVS), which provides Spitzer IRAC 3.6and 4.5um imaging down to AB~23 for a total area of 18sq.deg., to probe massive galaxies out to z~6 within arepresentative cosmic volume. We focus on the 1.5 sq.deg.area inside the XMM-LSS field, where we combine SERVSwith VISTA-VIDEO ZYJHK_S data (down to AB~24 at H andK_S). We select extremely red galaxies as either those withH-m3.6>1.6 (HIEROs) and/or K_S-m4.5>1.6 (KIEROs), andcalculate their photometric redshifts and stellar populationproperties using different stellar population models andfitting codes. We find that (H/K)IEROs have a redshiftdistribution that covers z~1-6; are massive (medianlog(Mstar/Msun)=10.8); and dusty (median E(B-V)=0.4).They have significant star-formation rates (typically

10-100Msun/yr) based on both our stellar population fittingand the fact that ~50% have MIPS24\um and/orSPIRE250um detections. A comparison with recent stellarmass function estimates, suggests that (H/K)IERO samplescontain a large fraction of the Mstar>10^11Msun galaxiesat z~2-5. Our study also reveals five z>5 candidates, allwith Mstar>10^11Msun. Our results suggest that, over thefull area of overlap between SERVS and VIDEO, we will find>10,000 (H/K)IEROs, including a few tens of z>5 massivegalaxies, allowing an exceptional probe into the build-up ofthe stellar mass in the universe.Author(s): Anna Sajina (Tufts University), Diego Capozzi (University ofPortsmouth), Mark Lacy (National Radio Astronomy Observatory), ClaudiaMaraston (University of Portsmouth), Janine Pforr (National OpticalAstronomy Observatory), Hugo Messias (Universidad de Concepcion),Duncan Farrah (Virginia Tech), Eduardo Gonzales-Solares (University ofCambridge), Matt Jarvis (Oxford University), Danilo Marchesini (TuftsUniversity), Lucia Marchetti (Padova University), Jean-Claude Mauduit(IPAC), Mattia Vaccari (Padova University)

207 – Arne Henden: Citizen Science in the Age of SurveysPlenary Session – America Ballroom North/Central – 03 Jun 2014 11:40 AM to 12:30 PMChair(s):Paula Szkody (Univ. of Washington)

207.01 – Citizen Science in the Age ofSurveysPaid professional astronomers are a new phenomenon -most of astronomical history has been written by amateurs.Modern technology has again leveled the playing field, withquality equipment, computers, software and the Internetgiving amateurs the ability to match or exceed the dataquality and quantity achievable by professionals. TheInternet in particular has come into play, with crowd-

sourcing through projects like Zooniverse, worldwideinstallation of private robotic observatories, and rapiddissemination of information leading the way. The futureonly shows more of these collaborative activities ahead, asall proposed surveys will require significant input fromcitizen scientists in order to achieve their goals. How thepublic is currently helping professional astronomers, howresearchers can get involved, and some of the futureopportunities will be presented.Author(s): Arne Henden (AAVSO)

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210 – On the Shoulders of Giants: Planets Beyond the Reach of Kepler II:DemographicsMeeting-in-a-Meeting – America Ballroom North/Central – 03 Jun 2014 02:00 PM to 03:30 PM

What kind of planets lie at orbit radii of 1-2 AU - beyond the reach of Kepler? In the last two decades we haveexplored a large sample of RV-detected and transit-detected planets, discovered distant planets with microlensingand several hot young planets at large radii using direct imaging, as well as the debris disks that provide clues toformation and evolution. In these 4 sessions, we explore the near future, and how we can expect to learn muchmore about the demographics and properties of cold outer planets. WFIRST-AFTA will open up this area, with amicrolensing survey to probe the population of long-orbit planets, and coronagraphy to take images and spectraof large planets in orbits at a few AU. Session II covers the demographics of the exoplanet population, based onwhat we know from RV surveys, Kepler, direct imaging, and microlensing.

Chair(s):Christopher Stark (Carnegie Institution of Washington)

Organizer(s):Stephen Unwin (JPL)

210.01 – Demographics of Giant Planets--Insights from TheoryThe demographics of giant planets arise from acombination of the physical properties and evolution ofprotoplanetary disks, the planet formation process itself,and the dynamical evolution of planets post-formation. Inthis talk, I will review each of these contributions to giantplanet demographics with an emphasis on how futurediscoveries can be used to separate and constrain theireffects. I will particularly discuss how giant planetdemographics will constrain the mechanism by which giantplanets form, an old theoretical problem on the cusp of anobservational breakthrough.Author(s): Ruth Murray-Clay (Harvard-Smithsonian Center forAstrophysics)

210.02 – Characterizing Cold Giant Planetsin Reflected Light: Lessons from 50 Years ofOuter Solar System Observation andExplorationA space-based coronagraph, whether as part of theWFIRST/AFTA mission or on a dedicated space telescopesuch as Exo-C or -S concepts, will be able to obtainphotometry and spectra of multiple giant planets aroundnearby stars, including many known from radial velocitydetections. Such observations will constrain the masses,atmospheric compositions, clouds, and photochemistry ofthese worlds. Giant planet albedo models, such as those ofCahoy et al. (2010) and Lewis et al. (this meeting), will becrucial for mission planning and interpreting the data.However it is equally important that insights gleaned fromdecades of solar system imaging and spectroscopy of giantplanets be leveraged to optimize both instrument designand data interpretation. To illustrate these points we willdraw on examples from solar system observations, by bothHST and ground-based telescopes, as well as by Voyager,Galileo, and Cassini, to demonstrate the importance clouds,photochemical hazes, and various molecular absorbers playin sculpting the light scattered by solar system giantplanets. We will demonstrate how measurements of therelative depths of multiple methane absorption bands ofvarying strengths have been key to disentangling thecompeting effects of gas column abundances, variations incloud height and opacity, and scattering by high altitudephotochemical hazes. We will highlight both the successes,such as the accurate remote determination of theatmospheric methane abundance of Jupiter, and a fewfailures from these types of observations. These lessonsprovide insights into technical issues facing spacecraftdesigners, from the selection of the most valuable camerafilters to carry to the required capabilities of the flightspectrometer, as well as mission design questions such aschoosing the most favorable phase angles for atmosphericcharacterization.Author(s): Mark Marley (NASA Ames Research Center), HeidiHammel (AURA)

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210.03 – The Occurrence Rate of GiantPlanets around M-dwarf StarsThe TRENDS high-contrast imaging program is a dedicatedsurvey based at Keck Observatory that uses high-contrastimaging observations to follow-up stars showing long-termradial velocity accelerations. In this talk, I will present anew technique invented to determine the occurrence rateof gas giant planets on wide orbits (0-20 AU) aroundlow-mass stars.Author(s): Justin Crepp (Notre Dame), Benjamin Montet (Harvard),John Johnson (Harvard), Andrew Howard (U. Hawaii), Geoffrey Marcy(Berkeley)

Contributing teams: California Planet Search

210.04 – Planet frequency beyond the snowline from MOA-II microlensing surveyGround-based microlensing surveys enable us to detectplanets down to Earth masses just beyond the snow line,where temperatures are cold enough for ices to condense.This area of the parameter space is not only out of reachfor Kepler but also a key part for planetary formation theorybecause the surface density of the proto-planetary diskincreases by a factor four to five beyond the snow line. It isthus important to understand the planet distributionbeyond the snow line. Giant planets located just beyondthe snow line also have been discovered by RV and directimaging, but detecting planets in this parameter spaceregion is still very difficult, in particular as we go down tothe super Earth regime. We present the result of thestatistical analysis of microlensing survey data byMicrolensing Observations in Astrophysics (MOA) during2007-2012. In this period, the MOA collaboration issued3300 microlensing alerts. Using the online data, we rejectevents with poor quality data and stellar binary lens events.Using these quality criteria, about 1500 single lens and 20planetary candidate events remain and are used for thestatistical analysis. In order to derive the planet abundance,an averaged number of planets per star, beyond the snowline, we calculate the detection efficiency for planets ineach selected event. Using the calculated detectionefficiencies, we derive the planet mass-ratio function andplanet mass function. We calculate the planet abundancewithin the mass and semi-major axis ranges where our datahas sufficient sensitivity to detect planets. We will discussthe planet abundance and compare them with previousmicrolensing and RV results.Author(s): Daisuke Suzuki (Osaka University)

Contributing teams: MOA collaboration

210.05 – Free-floating planets frommicrolensingGravitational microlensing has an unique sensitivity toexoplanets at outside of the snow-line and even exoplanetsunbound to any host stars because the technique does notrely on any light from the host but the gravity of the lens.MOA and OGLE collaborations reported the discovery of apopulation of unbound or distant Jupiter-mass objects,which are almost twice (1.8_{-0.8}^{+1.7}) as common asmain-sequence stars, based on two years of gravitationalmicrolensing survey observations toward the GalacticBulge. These planetary-mass objects have no host starsthat can be detected within about ten astronomical units bygravitational microlensing. However a comparison withconstraints from direct imaging suggests that most of theseplanetary-mass objects are not bound to any host star. Thesuch short-timescale unbound planetary candidates havebeen detected with the similar rate in on-goingobservations and these groups are working to update theanalysis with larger statistics. Recently, there are alsodiscoveries of free-floating planetary mass objects by thedirect imaging in young star-forming regions and in themoving groups, but these objects are limited to massiveobjects of 3 to 15 Jupiter masses.They are more massivethan the population found by microlensing. So they may bea different population with the different formation process,either similar with that of stars and brown dwarfs, orformed in proto-planetary disks and subsequently scatteredinto unbound or very distant orbits. It is important to fill thegap of these mass ranges to fully understand thesepopulations. The Wide Field Infrared Survey Telescope(WFIRST) is the highest ranked recommendation for a largespace mission in the recent New Worlds, New Horizons(NWNH) in Astronomy and Astrophysics 2010 DecadalSurvey. Exoplanet microlensing program is one of theprimary science of WFIRST. WFIRST will find about 3000bound planets and 2000 unbound planets by the highprecision continuous survey 15 min. cadence. WFIRST cancomplete the statistical census of planetary systems in theGalaxy, from super-Earths beyond the snow-line togravitationally unbound planets – a discovery spaceinaccessible to other exoplanet detection techniques.Author(s): Takahiro Sumi (Osaka University)

Contributing teams: MOA collaboration

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211 – Solar Surface and Interior IIMeeting-in-a-Meeting – America Ballroom South – 03 Jun 2014 02:00 PM to 03:30 PMChair(s):Jason Jackiewicz (New Mexico State University)

211.01D – The Dynamic Evolution of Active-Region-Scale Magnetic Flux Tubes in theTurbulent Solar Convective EnvelopeThe manner by which bundles of magnetic field, or fluxtubes, traverse the convection zone to eventual emergenceat the solar surface is not well understood. To provide aconnection between dynamo-generated magnetic fieldsand sunspots, I have performed simulations of magneticflux emergence through the bulk of a turbulent, solarconvective envelope by employing a thin flux tube modelsubject to interaction with flows taken from a hydrodynamicconvection simulation computed through the AnelasticSpherical Harmonic (ASH) code. Through performing thesesimulations, much insight has been gained about theinfluence of turbulent solar-like convection on the fluxemergence process and resulting active region properties. Ifind that the dynamic evolution of flux tubes change fromconvection dominated to magnetic buoyancy dominated asthe initial field strength of the flux tubes increases from 15kG to 100 kG. Additionally, active-region-scale flux tubes of40 kG and greater exhibit properties similar to those ofactive regions on the Sun, such as: tilt angles, rotationrates, and morphological asymmetries. The joint effect ofthe Coriolis force and helical motions present in convectiveupflows help tilt the apex of rising flux tubes toward theequator in accordance with Joy’s Law. Additionally,rotationally aligned, columnar convective structures calledgiant cells present in the ASH simulation organizes fluxemergence into a large-scale longitudinal pattern similar tothe active longitude trend on the Sun and other solar-likestars. The effect of radiative diffusion across the radiationzone-convection zone interface on the buoyant rise ofmagnetic flux tubes is also studied, as well as thepossibility of an induced twist of flux tube magnetic fieldslines due to the Coriolis force induced tilting of the flux tubeapex, presence of turbulent convection, and theconservation of helicity. Flux emergence simulationsthrough the convection zone of a Sun rotating at 5 timesthe current solar rate are also conducted to explore therotation-convection relationship as it relates to fluxemergence.Author(s): Maria Weber (High Altitude Observatory), Yuhong Fan(High Altitude Observatory), Mark Miesch (High Altitude Observatory)

211.02 – A Possible Role of Neutrinos inStimulating Beta Decays and itsSignificance for Solar PhysicsWe find evidence from measurements of Ag108, Ba133,Eu152, Eu154, Ra226 and Sr90 (Physikalisch-TechnischeBundesanstalt, Germany), Rn222 (Geological Survey ofIsrael), Co60, Pu239, and Sr90 (Lomonosov Moscow StateUniversity, Russia), Cl36 and Si32 (Brookhaven NationalLaboratory, USA) and Mn54 (Purdue University, USA) thatbeta-decay rates tend to be variable, and that the Sun isresponsible for some – perhaps all – of the variability. Onevariation is an annual oscillation with amplitude about 0.1%and maximum in January or February, presumably relatedto the annually varying Sun-Earth distance. We also findevidence for two rotational modulations, one with ameasured (synodic) frequency of about 12.5 year-1 (anabsolute, sidereal frequency of 13.5 year-1), due perhaps toprocesses in the radiative zone, and another with a synodicfrequency of about 11 year-1 (12 year-1 sidereal), dueperhaps to processes in an inner tachocline between thecore and the radiative zone. A steep gradient in angularvelocity (as in a tachocline) is known to be unstable andgenerate r-mode oscillations. These may be detectable asRieger-type oscillations in the outer tachocline, and tosimilar oscillations (with correspondingly lower frequencies,in proportion to the sidereal rotation frequencies) in theinner tachocline. We find evidence for such r-modeoscillations not only in beta-decay data, but also in solardiameter data. A possible explanation of the apparentbeta-decay variability is that decays may be stimulated byneutrinos. Since the flavor composition of the neutrino fluxcan be modified by the Sun’s internal magnetic field (viaResonant Spin Flavor Precession), magnetohydrodynamicprocesses in the deep solar interior may be detectable onEarth as neutrino-stimulated beta-decay fluctuations.Experiments suggest that a nuclide such as 32Si has abeta-decay-equivalent-cross-section of order 10-25 cm2,larger than the neutrino-equivalent-cross-section of anelectron or proton by about 1019. If this proves to becorrect, then less than 1 picogram of 32Si would yield thesame solar-neutrino-induced event rate as the Super-Kamiokande Observatory.Author(s): Peter Sturrock (Stanford Univ.), Ephraim Fischbach(Purdue University), Jere Jenkins (Texas A&M), Gideon Steinitz (GeologicalSurvey of Israel)

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211.03 – From the Tachocline Into theHeliosphere: Coupling a 3D kinematicdynamo to the CCMCDuring the last decade, axisymmetric kinematic dynamomodels have contributed greatly to our understanding ofthe solar cycle. However, with the advent of more powerfulcomputers the limitation to axisymmetry has been lifted.Here we present a 3D kinematic dynamo model whereactive regions are driven by velocity perturbationscalibrated to reproduce observed active region properties(including the size and flux of active regions, and thedistribution of tilt angle with latitude), resulting in a moreconsistent treatment of flux-tube emergence in kinematicdynamo models than artificial flux deposition. Wedemonstrate how this technique can be used to assimilateactive region observations obtained from the US NationalSolar Observatory/Kitt Peak (NSO/KP) synopticmagnetograms and how our model couples naturally withheliospheric models, paving the way for the simultaneousstudy of the evolution of the magnetic field in the solarinterior as well as its impact on the heliosphere.Author(s): Andres Munoz-Jaramillo (University of California),Anthony Yeates (Durham University), Petrus Martens (Montana StateUniversity), Edward DeLuca (Harvard-Smithsonian Center for Astrophysics)

211.04 – Towards a Unified Simulation ofConvective Dynamo Action and FluxEmergence in the SunOur global 3D simulations of convection and dynamo actionin a Sun-like star reveal that persistent wreaths of strongmagnetism can be built within the bulk of the conventionzone. Our recent simulations have achieved sufficientlyhigh levels of turbulence to permit portions of thesewreaths to become magnetically buoyant and rise throughthe simulated convective layer through a combination ofmagnetic buoyancy and advection by convective giantcells. Here we examine the characteristics of buoyantmagnetic structures that are self-consistently created bydynamo action and turbulent convective motions. Thesebuoyant loops originate within sections of the magneticwreaths in which turbulent flows amplify the fields to muchhigher values than is possible through laminar processes.Examining many such loops over a simulated magneticactivity cycle, we measure statistical trends in the polarity,twist, and tilt of these loops that mimic Hale’s Law, Joy’sLaw, and the hemispheric helicity rule observed insunspots. We further show that these magnetic structuresare primarily generated by non-axisymmetric turbulentamplification on timescales of about 15 days and not by the?-effect which primarily generates the large-scale wreaths.Author(s): Nicholas Nelson (Los Alamos National Laboratory),Benjamin Brown (UC-Santa Barbara), Mark Miesch (National Center forAtmospheric Research), Juri Toomre (Univ. of Colorado)

211.05 – Insights on the solar dynamo fromstellar observationsA successful dynamo model should not only explain thebroad characteristics of the magnetic field cycle for the Sun(22-year sunspot cycle with polarity reversals, migration ofactive latitudes toward the poles throughout the cycle, andJoy’s law), but should also be able to explain the cyclingbehavior observed in Solar-analog stars, which are veryclose to the Sun in essential characteristics. Our aim is todevelop a set of constraints on dynamo models from theobserved behavior of solar-analog stars obtained from anumber of long-running synoptic surveys of cycling activity(Mount Wilson Observatory HK survey, Lowel ObservatorySolar-Stellar Spectrograph, and the Fairborn ObservatoryAutomatic Photoelectric Telescope survey), in conjuncturewith stellar rotation and differential rotation data obtainedby the Kepler Mission and other sources. By carefullypiecing together the best data available today, we willprovide an improved understanding of the parameter spacein which Solar-like dynamos operate.Author(s): Ricky Egeland (Montana State University), PetrusMartens (Montana State University), Philip Judge (High AltitudeObservatory)

211.06 – Solar/Stellar Granulation as theKey Lower Boundary Condition for CoronalHeating and Wind AccelerationMuch of the hot plasma that eventually becomes thesupersonic solar wind appears to have its origin in small(100 km diameter) magnetic flux tubes that sit in thedownflowing lanes between convective granules in theSun's photosphere. Convective overturning motions jostlethese flux tubes and induce kink-mode oscillations that cangrow into Alfven waves in the corona. A great deal of recentwork has been done to explore how these Alfvenicfluctuations may drive a turbulent cascade, heat theplasma by gradual dissipation, and provide directacceleration to a wind via wave pressure gradients. Thispresentation will outline this work and show how anaccurate description of granulation is a key input toself-consistent models of coronal heating and solar windacceleration. These self-consistent models have also beenapplied successfully to predicting: (1) high-energy emissionfrom accreting T Tauri stars, (2) the mass loss rates of cooldwarfs and red giants, and (3) the combined X-ray, radio,and submillimeter emission from a young nearby M dwarf.In addition, a recent analysis of stellar granulation withKepler photometry has shown that our understanding of theshallow convection zones of F-type stars still requiresadditional refinement. In all cases, the combination ofmultiple types of observational data has been crucial toimproving our understanding. For the Sun, thenext-generation capabilities of ATST/DKIST are expected toprovide much more precise knowledge about this importantlower boundary condition to the heliosphere.Author(s): Steven Cranmer (Harvard-Smithsonian CfA)

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212 – CME IMeeting-in-a-Meeting – Staffordshire – 03 Jun 2014 02:00 PM to 03:30 PMChair(s):Sophie Masson (NASA/GSFC)

212.01 – The Rayleigh-Taylor Instability andthe role of Prominences in theChromosphere-Corona Mass CycleWe review recent results in the study of so-called"prominence bubbles", a buoyant instability discovered inquiescent solar prominences by the Hinode/SOT instrumentin 2007. Analysis of the plasma flows along the boundary ofthe bubbles indicates that shear flows leading to Kelvin-Helmholtz instability waves can develop into the seedperturbations triggering the Rayleigh-Taylor instability. Thenon-linear phase of the RT instability leads to the formationof large turbulent plumes that transport the bubble plasma(and presumably magnetic flux) into the overlying coronalflux rope. We propose that the upward turbulent transportof hot bubble plasma and the downflows of coolerchromospheric plasma in the prominence are relatedaspects of a large-scale "chromosphere-corona mass cycle"in which hot plasma and magnetic flux and helicity from thechromosphere are transported upwards while the coolerprominence plasma downflows, which decouple from themagnetic field they are originally frozen-into, represent thecondensation return flows of the cycle. This cycling enablesa mechanism by which magnetic flux and helicity build upin the coronal flux rope while mass drains out of the fluxrope, eventually triggering a "loss of confinement" eruptionin the form of a CME.Author(s): Thomas Berger (National Solar Observatory), Wei Liu(Stanford Lockheed Institute for Space Research), Andrew Hillier (KyotoUniversity), Eamon Scullion (Trinity College), Boon Chye Low (High AltitudeObservatory)

212.02 – New Aspects of a Lid-RemovalMechanism in the Onset of a SEP-ProducingEruption SequenceWe examine a sequence of two ejective eruptions from asingle active region on 2012 January 23, usingmagnetograms and EUV images from SDO/HMI andSDO/AIA, and EUV images from STEREO. Cheng et al.(2013) showed that the first eruption's (``Eruption 1'') fluxrope was apparent only in ``hotter'' AIA channels, and thatit removed overlying field that allowed the second eruption(``Eruption 2'') to begin via ideal MHD instability; here wesay Eruption 2 began via a ``lid removal'' mechanism. Weshow that during Eruption-1's onset, its flux rope underwent``tether weakening'' (TW) reconnection with the field of anadjacent active region. Standard flare loops from Eruption 1developed over Eruption-2's flux rope and enclosedfilament, but these overarching new loops were unable toconfine that flux rope/filament. Eruption-1's flare loops,from both TW reconnection and standard-flare-modelinternal reconnection, were much cooler than Eruption-2'sflare loops (GOES thermal temperatures of ~9 MKcompared to ~14 MK). This eruption sequence produced astrong solar energetic particle (SEP) event (10 MeV protons,>10^3 pfu for 43 hrs), apparently starting whenEruption-2's CME blasted through Eruption-1's CME at5---10 R_s. This occurred because the two CMEs originatedin close proximity and in close time sequence: Eruption-1'sfast rise started soon after the TW reconnection; the lidremoval by Eruption-1's ejection triggered the slow onset ofEruption 2; and Eruption-2's CME, which started ~1 hr later,was three times faster than Eruption-1's CME.Author(s): Alphonse Sterling (NASA/MSFC), Ronald Moore(NASA/MSFC), David Falconer (NASA/MSFC), Javon Knox (Norfolk StateUniversity)

212.03 – MHD simulations of homologousand cannibalistic coronal mass ejectionsWe present magneto-hydrodynamic simulations of thedevelopment of a homologous sequence of coronal massejections (CMEs) and demonstrate their so-calledcannibalistic behavior. These CMEs originate from therepeated formations and partial eruptions of kink unstableflux ropes as a result of the continued emergence of atwisted flux rope across the lower boundary into apre-existing coronal potential arcade field. The simulationsshow that a CME erupting into the open magnetic fieldcreated by a preceding CME has a higher speed, andtherefore tends to be cannibalistic, catching up andmerging with the preceding one into a single fast CME. Allthe CMEs attained speeds of about 1000 km/s as they exitthe domain. The reformation of a twisted flux rope aftereach CME eruption during the sustained flux emergencecan naturally explain the X-ray observations of repeatedreformations of sigmoids and “sigmoid-under-cusp”configurations at a low-coronal source of homologousCMEs.Author(s): Yuhong Fan (HAO/NCAR), Piyali Chatterjee (HAO/NCAR)

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212.04 – A Method for Embedding CircularForce-Free Flux Ropes in Potential MagneticFieldsWe propose a method for constructing approximateforce-free equilibria in pre-eruptive configurations thatlocally are a bipolar-type potential magnetic field with athin force-free flux rope embedded inside it. The flux rope isassumed to have a circular-arc axis, circular cross-section,and electric current that is either concentrated in a thinlayer at the boundary of the rope or smoothly distributedacross it with a maximum of the current density at thecenter. The entire solution is described in terms of themagnetic vector potential in order to facilitate theimplementation of the method in numericalmagnetohydrodynamic (MHD) codes that evolve the vectorpotential rather than the magnetic field itself. Theparameters of the flux rope can be chosen so that itssubsequent MHD relaxation under photospheric line-tiedboundary conditions leads to nearly exact numericalequilibria. To show the capabilities of our method, we applyit to several cases with different ambient magnetic fieldsand internal flux-rope structures. These examplesdemonstrate that the proposed method is a useful tool forinitializing data-driven simulations of solar eruptions.Author(s): Viacheslav Titov (Predictive Science, Inc.), Tibor Torok(Predictive Science, Inc.), Zoran Mikic (Predictive Science, Inc.), Jon Linker(Predictive Science, Inc.)

212.05 – A plasma ? transition within apropagating flux ropeWe present a 2.5D MHD simulation of a magnetic flux rope(FR) propagating in the heliosphere and investigate thecause of the observed sharp plasma ? transition.Specifically, we consider a strong internal magnetic fieldand an explosive fast start, such that the plasma ? issignificantly lower in the FR than the sheath region that isformed ahead. This leads to an unusual FR morphology inthe first stage of propagation, while the more traditionalview (e.g. from space weather simulations like Enlil) of a`pancake' shaped FR is observed as it approaches 1AU. Weinvestigate how an equipartition line, defined by amagnetic Weber number, surrounding a core region of apropagating FR can demarcate a boundary layer wherethere is a sharp transition in the plasma ?. The substructureaffects the distribution of toroidal flux, with the majority ofthe flux remaining in a small core region which maintains aquasi-cylindrical structure. Quantitatively, we investigate alocus of points where the kinetic energy density of therelative inflow field is equal to the energy density of thetransverse magnetic field (i.e. effective tension force). Thesimulation provides compelling evidence that at allheliocentric distances the distribution of toroidal magneticflux away from the FR axis is not linear; with 80% of thetoroidal flux occurring within 40% of the distance from theFR axis. Thus our simulation displays evidence that thecompeting ideas of a pancaking structure observedremotely can coexist with a quasi-cylindrical magneticstructure seen in situAuthor(s): Neel Savani (NASA GSFC), Angelos Vourlidas (NavalResearch Laboratory), Daikou Shiota (Nagoya University), Mark Linton(Naval Research Laboratory), Kanya Kusano (Nagoya University), NoeLugaz (University of New Hampshire), Alexis Rouillard (Universit deToulouse)

212.06 – Rapid CME Cavity Formation andExpansionA cavity is supposed to be a general feature ofwell-developed CMEs at the stage they can be imaged bywhite-light coronagraphs (in the outer corona and solarwind). The cavity is interpreted as the cross section of theCME flux rope in the plane of sky. Preexisting cavities areobserved around some quiescent erupting prominences,but usually not in active regions. Observations of CMEcavities in the inner corona, where most of them appear toform, have become possible only with the STEREO and SDOmissions. These reveal a very rapid formation andexpansion of "EUV cavities" in fast and impulsivelycommencing eruptions early in the phase of main CMEacceleration and impulsive flare rise. Different from thewhite-light observations, the EUV cavity initially appears tobe larger than the CME flux rope. However, it evolves intothe white-light cavity subsequently. MHD simulations of fluxrope eruptions conform to this picture of initially largercavity but subsequently approaching cavity and flux ropesize. The initial expansion of ambient flux can beunderstood as a "reverse pinch effect", driven bydecreasing flux rope current as the rope rises.Author(s): Bernhard Kliem (University of Potsdam), Terry Forbes(University of New Hampshire), Spiros Patsourakos (University ofIoannina), Angelos Vourlidas (Naval Research Laboratory)

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213 – The Galactic Center and Nearby GalaxiesOral Session – St. George AB – 03 Jun 2014 02:00 PM to 03:30 PMChair(s):Rafael Martinez

213.01 – Winds from the S-Star ClusterReduce the Accretion Rate onto Sgr A*High-resolution radio continuum images of the region withina few arcseconds of Sgr A* at wavelengths of 7 and 12 mmshow three new radio structures. One is a 2-3'' hollowteardrop-shaped structure centered on Sgr A*. Highlyblue-shifted [NeII] and [FeIII] line emission is detected alongthe boundary of this teardrop-shaped bubble, ~2.2'' southof Sgr A*. The second structure is a faint, incomplete ringsurrounding Sgr A* with typical surface brightness at 7 mmof ~0.1 mJy per ~0.04'' x 0.08'' beam. This partial ringcoincides with the outer boundary of the S-star clusterwhich consists of ~30 B dwarfs orbiting within 1'' of Sgr A*.Lastly, on a scale of ~20'' to the N of Sgr A*, a balloon-shaped structure is detected. We interpret that the newmorphological and kinematic structures result from thedynamical effects of a combined cluster wind. This wind iscreated at a rate ~3 x 10^{-5} solar mass per year by themerging of individual stellar winds from the B stars in theS-star cluster. What is significant about this interpretation isthat the expanding wind excludes the shocked winds fromO and WR stars in the central parsec of the Galaxy.Meanwhile Sgr A* accretes material from within the Scluster at a rate less than or equal 3 x 10^{-7} solar massper year, thus explaining the low luminosity of Sgr A*without the ejection of a large fraction of the accretedmaterial.Author(s): Farhad Yusef-Zadeh (Northwestern Univ.), M. Wardle(Macquarie), D. Roberts (Northwestern Univ.), Daryl Haggard(Northwestern Univ.), John Lacy (University of Texas), Marc Royster(Northwestern Univ.), William Cotton (NRAO)

213.02D – Probing the Extreme Environmentof the Galactic Center with Observationsfrom SOFIA/FORCASTIn this thesis we present a study of the inner 40 pc of theGalactic center addressing the dense, dusty torus aroundSgr A*, dust production around massive stars, and massivestar formation. Observations of warm dust emission fromthe Galactic center were performed using the Faint ObjectInfrared Camera for the SOFIA Telescope (FORCAST). Adense, molecular torus referred to as the CircumnuclearDisk (CND) orbits Sgr A* with an inner radius of ~1.4 pc andextending to ~7 pc. The inner edge of the CND, which werefer to as the Circumnuclear Ring (CNR), exhibits featuresof a classic HII region and appears consistent with theprevailing paradigm in which the dust is heated by theCentral cluster of hot, young stars. We do not detect anystar formation occurring in the CNR; however, we reveal thepresence of density “clumps” along the inner edge of theCNR. These clumps are not dense enough to be stableagainst tidal shear from Sgr A* and will be sheared outbefore completing a full orbit (~10^5 yrs). Three LuminousBlue Variables (LBVs) are located in and near the QuintupletCluster 40 pc in projection from Sgr A*: qF362, the Pistolstar, G0.120-0.048 (LBV3). FORCAST observation reveal theasymmetric, compressed shell of hot dust surrounding thePistol Star and provide the first detection of the thermalemission from the symmetric, hot dust envelopesurrounding LBV3. However, no detection of hot dustassociated with qF362 is made. We argue that the Pistolstar and LBV3 are identical “twins” that exhibit contrastingnebulae due to the external influence of their differentenvironments. G-0.02-0.07, a complex consisting of threecompact HII regions and one ultracompact HII region, islocated at the edge of a molecular cloud 6 pc in projectionto the east of Sgr A* and contains the most recent episodeof star formation in the Galactic center. We probe the dustmorphology, energetics, and composition of the regions tostudy the star forming conditions of a molecular cloud inthe strong gravitational potential of Sgr A*.Author(s): Ryan Lau (Cornell University), Terry Herter (CornellUniversity), Mark Morris (UCLA), Joseph Adams (Cornell University), EricBecklin (UCLA)

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213.03 – Spitzer observations of Sgr A* andcloud G2The supermassive black hole at the center of our Galaxy isa fluctuating source of electromagnetic radiation derivedfrom its accretion flow. For the past decade, the blackhole’s ingestion has been modest, but its accretion rate andluminosity are predicted to surge as the cloud G2 swings byand feeds Sgr A* with a helping of fresh gas. We havestarted a program to monitor Sgr A* with Spitzer/IRAC at awavelength of 4.5 microns as the anticipated elevatedaccretion episode proceeds. Near-infrared wavelengths arewhere the black hole’s emission has been bestcharacterized in the past, and IRAC observations willcomplement planned observations with other observatoriesat X-ray, radio, and submillimeter wavelengths. Thevariability of Sgr A* is a random red-noise process, but thelimited duration of continuous ground-based observations(<6 hr) has prevented direct measurement of thecorrelation timescale. This timescale corresponds to athermal or viscous timescale associated with the innerradius of the accretion disk, and knowing it is critical for theblack hole accretion physics. The Spitzer observing plan isto monitor Sgr A* continuously at 4.5 microns for >23.5hours at each of six epochs. Epochs include one in 2013Dec, three more in 2014 Jun-Jul, and two more in 2014Nov-Dec. These will enable us to follow the initial stages ofwhat has been predicted to be an extended accretionepisode. In the 2013 Dec epoch we detected emission fromSgr A* in excess of the noise level for approximately 40% ofthe period observed, with individual maxima having peaklevels of 1-10 milliJanskys.Author(s): Joseph Hora (Harvard-Smithsonian, CfA), Giovanni Fazio(Harvard-Smithsonian, CfA), Steven Willner (Harvard-Smithsonian, CfA),Sean Carey (Spitzer Science Center), James Ingalls (Spitzer ScienceCenter), Matthew Ashby (Harvard-Smithsonian, CfA), Eric Becklin (SOFIAScience Center), Andrea Ghez (UCLA), Leo Meyer (UCLA), Mark Morris(UCLA), Howard Smith (Harvard-Smithsonian, CfA), Gunther Witzel (UCLA),Jiasheng Huang (Harvard-Smithsonian, CfA), Zhong Wang (Harvard-Smithsonian, CfA)

213.04 – Leptonic v.s. Hadronic Origin of theGamma-ray Emission of the Fermi bubbles:Updates from Fermi-LAT and Forecast forFuture Gamma-ray TelescopesData from the Fermi-LAT revealed two large gamma-raybubbles, extending 50 degrees above and below theGalactic center, with a width of about 40 degrees inlongitude. Such structure has been confirmed with multi-wavelength observations. With the most up to dateFermi-LAT data analysis, I will show that the Fermi bubbleshave a spectral cutoff at both low energy < 1 GeV and highenergy > 150 GeV. Detailed analysis of the spectralfeatures will help us to distinguish the leptonic origin fromhadronic origin of the gamma-ray emission from thebubbles. I will also describe what we expect to learn aboutthe bubbles from future gamma-ray telescopes after Fermi,with an emphasis on Dark Matter Particle Explorer and PairProduction Gamma-ray Unit.Author(s): Meng Su (MIT)

213.05 – Tidal Streams Near and FarThe Pandas survey of stars in M31's disk and halo iscrisscrossed by numerous tidal features from both M31 andthe Milky Way. Here I focus on two narrow stellar streamsvisible in the survey. They have comparable angular extentin the survey (10-13 degrees long versus only 0.3 degreewide), but one is a local Milky Way stream at about 30 kpcand one is in M31, roughly 25 times more distant. Iestimate the stellar mass and metallicity in the streamsand the distance gradient along them. The kinematics ofthe M31 stream is sparsely sampled by red giant stars andglobular clusters. Bayesian modeling of the stream datayields accurate constraints on the orbital parameters of thestreams.Author(s): Mark Fardal (University of Massachusetts)

Contributing teams: PAndAS

213.06 – The black hole mass at the centerof NGC 5419We measured the black hole mass at the center of themassive core elliptical NGC 5419 using SINFONI adaptiveoptics spectra combined with SALT long slit kinematics. Wedetect an elongated blue central structure, possibly a diskof young stars orbiting the black hole.Author(s): Gary Wegner (Dartmouth College), X. Mazzalay(Max-Planck Institut fuer extraterrestrische Physik), Jens Thomas(Max-Planck Institut fuer extraterrestrische Physik), Roberto Saglia(Max-Planck Institut fuer extraterrestrische Physik), Ralf Bender(Max-Planck Institut fuer extraterrestrische Physik), Peter Erwin(Max-Planck Institut fuer extraterrestrische Physik), M. Fabricius(Max-Planck Institut fuer extraterrestrische Physik), M. Nowak (Max-PlanckInstitut fuer extraterrestrische Physik)

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214 – Bridging Laboratory and Astrophysics: PlanetaryMeeting-in-a-Meeting – St. George CD – 03 Jun 2014 02:00 PM to 03:30 PM

Laboratory astrophysics is the Rosetta Stone that enables astronomers to understand and interpret the cosmos.This session will focus on the interplay between astrophysics with theoretical and experimental studies into theunderlying planetary science processes, which drive our Universe.

Chair(s):Farid Salama (NASA Ames Research Center)

214.01 – Haze Formation in PlanetaryAtmospheres: Lessons from the LabFor more than 50 years, haze formation in planetaryatmospheres has been simulated in the laboratory. Ofparticular interest are simulations of haze formation in theatmosphere of Titan, the largest moon of Saturn. Thesesimulation experiments have provided a wealth ofknowledge about the possible composition and opticalproperties of haze particles, informed efforts to understandthe transition between gas phase and particle chemistry,and provide “analogue” materials to aid in the selectionand testing of the next generation of spacecraft basedanalytical techniques. In this talk I will review the currentstate of knowledge from Titan atmosphere simulationexperiments, discuss difficulties that have arisen fromknowledge gained from the Cassini-Huygens mission to theSaturn system, and present particular areas wherelaboratory studies could provide much needed guidance forthe observation and modeling communities studyingatmospheres in our solar system and beyond.Author(s): Sarah Horst (University of Colorado)

214.02 – Laboratory Astrophysics withPrimitive Extraterrestrial Materials: TheOrigin and Early Evolution of Our PlanetarySystemThe planets in our Solar System formed from aprotoplanetary disk of gas and dust, the solar nebula. Dueto billions of years of evolution, the planets themselves donot preserve many signatures of the earliest stages of theirformation. However, records of the nebula and of theearliest planetary formation epoch are preserved inasteroids and comets, and samples of these are availablefor laboratory study in the form of meteorites andinterplanetary dust particles, as well as asteroidal andcometary dust returned by spacecraft. Primitiveextraterrestrial materials contain pristine samples of theearliest solids that formed the building blocks of the planetsincluding both ‘’presolar’’ materials from prior generationsof stars and the interstellar medium as well as early-formedsolar nebular dust. Detailed laboratory analyses (e.g.,isotopic, elemental and microstructural studies) of thesematerials provide unique insights into a wide range ofastrophysical processes, including stellar nucleosynthesis,galactic chemical evolution, interstellar dust processing andchemistry, and mixing and accretion processes inprotoplanetary disks. This talk will review many of thesetopics with a focus on how meteorites constrain theastrophysical setting for solar system formation, thestarting materials of the planets, timescales of planetformation, and the origin and distribution of water andcarbon, the essential ingredients for life.Author(s): Larry Nittler (Carnegie Inst. Of Washington )

214.03 – Optical Constants of the Methane-Nitrogen Binary Ice System: Implications forMethane-Dominated TransneptunianObjectsPluto, Eris, and Makemake, unlike most Transneptunianobjects (TNOs) with water-ice rich or featureless surfaces(Barucci et al., 2008), display infrared spectra dominatedby methane ice (Brown, 2008). These three TNOs are oftencompared with Neptune's large satellite Triton, since itsspectrum is similarly dominated by methane ice and it isthought to have formed similarly to Pluto, Eris, andMakemake, prior to its capture into a retrograde orbitaround Neptune. In addition to methane ice, nitrogen icehas been directly detected on Pluto and Triton via the 2.148micron absorption band (Cruikshank et al., 1984; Owen etal., 1993). Thermodynamic equilibrium dictates that ifmethane and nitrogen ices are both present, for most of therange of possible nitrogen/methane relative abundances,two distinct phases must coexist at temperatures relevantto the surfaces of these icy dwarf planets (Prokhvatilov andYantsevich, 1983; Lunine and Stevenson, 1985): methaneice saturated with nitrogen and nitrogen ice saturated withmethane. We present infrared absorption coefficientspectra in the wavelength range 0.8 - 2.5 micron ofmethane diluted in nitrogen and nitrogen diluted inmethane at temperatures between 40 and 90 K and atdifferent mixing ratios, allowing a proper model to beconstructed for any TNO where the methane/nitrogen ratiofalls between the two solubility limits such that both phasesare present.Author(s): Silvia Protopapa (Department of Astronomy Universityof Maryland), William Grundy (Lowell Observatory), Stephen Tegler(Department of Physics and Astronomy, Northern Arizona University),Justin Bergonio (Department of Physics and Astronomy, University ofHawai'i)

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214.04 – The THS experiment: probingTitan's atmospheric chemistry at lowtemperatureIn Titan’s atmosphere, a complex chemistry between N2and CH4 occurs at temperatures lower than 200K and leadsto the production of heavy molecules and subsequentlysolid aerosols that form the haze surrounding Titan. TheTitan Haze Simulation (THS) experiment has beendeveloped at the NASA Ames COSmIC facility to studyTitan’s atmospheric chemistry at low temperature in orderto help interpret Cassini’s observational data. In the THS,the chemistry is simulated by plasma in the stream of asupersonic expansion. With this unique design, the gas isjet-cooled to Titan-like temperature (~150K) beforeinducing the chemistry by plasma, and remains at lowtemperature in the plasma discharge (~200K). DifferentN2-CH4-based gas mixtures can be injected in the plasma,with or without the addition of heavier precursors presentas trace elements on Titan. Both the gas phase and solidphase products resulting from the plasma-inducedchemistry can be monitored and analyzed using acombination of complementary in situ and ex situdiagnostics. Here we present the complementary results oftwo studies of the gas and solid phase. A Mass

spectrometry analysis of the gas phase has demonstratedthat the THS experiment is a unique tool to probe the firstand intermediate steps as well as specific chemicalpathways of Titan’s atmospheric chemistry at Titan-liketemperature. The more complex chemistry, observed in thegas phase when adding trace elements to the initialN2-CH4 mixture, has also been confirmed by an extensivestudy of the solid phase products: Scanning ElectronMicroscopy images have shown that aggregates producedin N2-CH4-C2H2-C6H6 mixtures (up to 5 ?m in diameter)are much larger than those produced in N2-CH4 mixtures(0.1-0.5 ?m), and Nuclear Magnetic Resonance resultssupport a growth evolution of the chemistry when addingacetylene to the N2-CH4 mixture, resulting in theproduction of more complex hydrogen bonds than with asimple N2-CH4 mixture. These complementary studiesshow the high potential of THS to better understand Titan’schemistry and the origin of aerosol formation.Acknowledgments This research is supported by NASA SMDPATM.Author(s): Ella Sciamma-O'Brien (Bay Area EnvironmentalResearch Institute), Kathleen Upton (California Institute of Technology),Jack Beauchamp (California Institute of Technology), Farid Salama (NASAAmes Research Center)

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215 – Star Formation and Interstellar MediumOral Session – Gloucester, 2nd Floor – 03 Jun 2014 02:00 PM to 03:30 PMChair(s):Julia Roman-Duval (Space Telescope Science Institute)

215.01 – Pressure in the Diffuse InterstellarMedium from Observations of CO and [CII]The pressure of the diffuse interstellar medium plays animportant role in determining the balance betweendifferent regions, the formation and evolution of interstellarclouds, and possibly regulating star formation. We herereport use of UV absorption data of CO taken from theliterature and [CII] observations taken with Herschel todetermine the thermal pressure of diffuse line of sightclouds. An average value in the range 5000 - 6000 K/cm3characterizes both sets of observations, somewhat higherthan generally found in the literature.Author(s): Paul Goldsmith (JPL), Maryvonne Gerin (LERMA & ENS)

215.02 – Gas Kinematics in FilamentaryInfrared Dark CloudsMany infrared dark clouds (IRDCs) have filamentarystructures, and some of them present converging filamentsto a central hub, known as hub-filament systems (HFSs).These filaments could play a crucial role in feeding gas tothe star forming regions at the hub. With the SubmillimeterArray in the compact and sub-compact configurations, weconducted a mini-survey of five high-mass (>10^3 Msolar)HFSs, and obtained the dust emission and spectra lines at1.3 mm. We found filamentary structures in both dustcontinuum and spectral line emission, with a characteristicwidth of 0.1 pc and length of 1 pc. The dust emission isconsistent with the infrared extinction features, indicatingthe existence of dense and cold gas, while massive dustcores are usually associated with the hubs. Complexorganic molecules including CH3OH are found towards thedust cores. In particular, optically-thin intermediate densitygas tracers, such as C18O, reveal a possible trend of gasinfall along filaments towards hubs. This is consistent withthe scenario that dense gas is accreted onto dense coresthrough filaments and form high-mass star clusters.Author(s): Xing Lu (Harvard-Smithsonian Center for Astrophysics),Qizhou Zhang (Harvard-Smithsonian Center for Astrophysics), Hauyu Liu(Academia Sinica Institute of Astronomy and Astrophysics)

215.03 – Diagnosing the Star FormationRate in Massive Galactic Star FormingRegionsIn extragalactic studies many different observables areused to trace the star formation history averaged overgalaxy or kiloparsec scales. By studying star formation inour Galaxy we are able to resolve individual sources anddirectly count up the young stars in a star forming complex.The star formation rates that are determined from thismethod rely on the input assumptions. I will describe howdifferent assumptions and variables alter the derived starformation rate for a sample of massive galactic star formingregions and how these star formation rates compare tothose derived using methods developed in the study ofexternal galaxies.Author(s): Sarah Willis (Iowa State University), Massimo Marengo(Iowa State University), Howard Smith (Harvard-Smithsonian CfA), LoriAllen (National Optical Astronomy Observatories), Andres Guzman(Harvard-Smithsonian CfA), Rafael Martinez (Harvard-Smithsonian CfA)

215.05 – Gaining Insight into StarFormation: Resolved Star Formation LawsUntil recently astronomers have used star formation laws tomeasure the star formation rate and star formationefficiency of galaxies only on global scales because of thepoor resolution of available data. What I am now capable ofproducing is a spatially resolved star formation law that canprovide direct insight into the physical processes thatgovern star formation and assess the short-term nature ofbursts of star formation and the longer-term nature oflarger-scale events that can dictate the global distributionof stars and the ultimate fate of a galaxy as a whole. I amusing exquisite narrowband optical data from a variety ofsources, including the Hubble Space Telescope, and KittPeak National Observatory, etc., in conjunction withinfrared data from the Spitzer Infrared Nearby GalaxySurvey and the Spitzer Local Volume Legacy survey, neutralgas data from The HI Nearby Galaxy Survey, and moleculargas data from the Berkeley-Illinois-Maryland AssociationSurvey of Nearby Galaxies, to provide star formation ratesand star formation efficiencies on previously inaccessiblesmall spatial scales across a suite of galaxies that representa range of star formation environments and scales. Mysample includes 18 spiral galaxies ranging from 2.1 to 15.1Mpc in distance and offers a large range of morphologicaltypes (i.e. a large range of star formation environments). Iam using these data to test different models of starformation modes under a variety of physical conditions andrelate the variations I observe to the known local physicalconditions and the associated star formation histories foreach locale within each galaxy. This is the heart of thematter – that the nature and evolution of the local physicalenvironment intimately influences how stars can form, howquickly and how massive those stars are allowed to form,and as a result how they shape the local conditions forsubsequent star formation. It is this tracking of the stellarecology that is vital for insight into the star formationprocess, but also to understand the conditions that canresult in star and planet formation, or conversely whatconditions prevent this. Such an analysis is only possiblewith the kind of datasets I am producing.Author(s): Kelley Liebst (Arizona State University), Paul Scowen(Arizona State University)

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215.06 – Galaxies on FIRE: Stellar FeedbackExplains Inefficient Star FormationMany of the most fundamental unsolved questions in starand galaxy formation revolve around star formation and"feedback" from both massive stars and accretion ontosuper-massive black holes. I'll present new simulationswhich attempt to realistically model the diverse physics ofthe interstellar medium, star formation, and feedback fromstellar radiation pressure, supernovae, stellar winds, andphoto-ionization. These mechanisms lead to 'self-regulated'galaxy and star formation, in which global correlations suchas the Schmidt-Kennicutt law and the global inefficiency ofstar formation -- the stellar mass function -- emergenaturally. Within galaxies, feedback regulates the structureof the interstellar medium, and many observed propertiesof the ISM, star formation, and galaxies can be understoodas a fundamental consequence of super-sonic turbulence ina rapidly cooling, self-gravitating medium. But feedbackalso produces galactic super-winds that can dramaticallyalter the cosmological evolution of galaxies, their behaviorin galaxy mergers, and structure of the inter-galacticmedium: these winds depend non-linearly on multiplefeedback mechanisms in a way that explains why theyhave been so difficult to model in previous "sub-grid"approaches.Author(s): Philip Hopkins (Caltech)

Contributing teams: The FIRE Team

215.07 – Star formation in interactinggalaxies: A tale of compactnessAt intermediate redshifts, a correlation has been found byMagnelli et al. between the dust temperature instar-forming galaxies, their specific star formation rate, andtheir distance from the so-called main sequence in theSFR-M* plane. This result has been interpreted in terms of adifference in the ISM physics between galaxies on and offthe main sequence. In this contribution we attempt tocharacterize the ISM physics in interacting systems withdifferent levels of specific star formation in terms of thecompactness parameter, which is related to the averageheating flux irradiated onto the dust particles surroundingindividual HII regions. We use CHIBURST, a Monte CarloBayesian algorithm to fit the multiwavelength SEDs of a setof simulated and observed nearby interactions from Lanz etal. 2014 and derive physical parameters of the ISM. We findthat compactness is related to the evolutionary stage of theinteractions: early interactions (older starbursts) have lowcompactness, whereas systems near coalescence (youngerstarbursts) have the highest possible compactness. Aftercoalescence, compactness decreases as the HII regionscontinue to expand without replenishment of hot dust bynew star formation activity. Interestingly, main sequencegalaxies show on average a smaller compactness ascompared to their starburst counterparts. This link betweenthe overall SED properties of starbursts and the internalphysics of the ISM at the HII region level is a promising toolin the characterization of unresolved starbursts, and pointsto a physically based definition of the main sequence ofstar formation in galaxies.Author(s): Juan Rafael Martinez-Galarza (SmithsonianAstrophysical Observatory), Lauranne Lanz (Caltech), ChristopherHayward (Max-Planck-Institut für Astronomie), Andreas Zezas (SmithsonianAstrophysical Observatory), Howard Smith (Smithsonian AstrophysicalObservatory), Matthew Ashby (Smithsonian Astrophysical Observatory),Chao-Ling Hung (Smithsonian Astrophysical Observatory)

215.08 – STAR CLUSTERS IN INTERACTINGGALAXIES : FORMATION AND EVOLUTIONGalaxy mergers are vast stellar nurseries where starclusters form, but the immense tidal disruption forces arealso at work, which causes destruction of the clustersystems. This simultaneous formation and destruction ofthe clusters leads to selective survival of clusters. Here, weinvestigate the formation and evolution of star clusters ininteracting galaxies using a suite of high-resolutionsmoothed particle hydrodynamics simulations. In thesimulations, star clusters are identified using the clusterfinding algorithm, the Amiga Halo Finder. We found that themass function of the star clusters change significantlyduring the course of galaxy merger, and the peak ofdensity probability distribution shifts from high mass to~7x10^5 Msun at late times. Furthermore, we found thatthe survived clusters are those that have the highestspecific binding energy. Our results suggest that high-massclusters are more easily destroyed than the low-mass ones,and that the observed peak of globular cluster massfunction at 3x10^5 Msun may be a result of such selectivesurvival of clusters.Author(s): Moupiya Maji (The Pennsylvania State University),Qirong Zhu (The Pennsylvania State University), Yuexing Li (ThePennsylvania State University), Jane Charlton (The Pennsylvania StateUniversity)

215.09 – Astrochemical Correlations inMolecular CloudsWe investigate the spectral correlations between differentchemical tracers used to observe molecular clouds. Westudy a 600 Solar Mass molecular cloud with Mach number6.6 modeled using the magnetohydrodynamic code ORION.The chemical abundances are calculated by 3D-PDR, athree-dimensional astrochemical code using a full networkof 3300 reactions and 215 species. We take syntheticobservations of 16 different species using the non-LTEradiative transfer code RADMC-3D. The effects of differentlines of sight and spatial resolution on the emission maps ofthe 16 different species will be discussed in this talk. Weuse the Spectral Correlation Function to quantify thestructure of the simulated cloud in position-position-velocityspace, which measures the average rms velocity betweenspectra separated by a given length scale. This statistic hasbeen shown to be sensitive to global hydrodynamicparameters, such as the sonic Mach number and velocitydispersion. The SCF is analytically fit by a power law, withthe slope being the one free parameter. We verify that theSCF is generally insensitive to the sightline through thecloud. We discover that the beam size has a distinct effecton different chemical tracers. However, the change is notlarge enough to move the SCF slopes into different parts ofthe parameter space. This is the first quantitative 3D studyof the spectral similarity of a variety of species. We predictthe observed SCF for a broad range of observationaltracers, and thus, identify complementary species. Inparticular, we show that the pairs C and CO, C+ and CN,NH3 and H2CS have very similar SCFs. The results from thisstudy will also give observers a guide for selecting whichchemical tracers would be best for observing differentlength scales.Author(s): Brandt Gaches (University of Massachusetts -Amherst), Stella Offner (University of Massachusetts - Amherst)

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216 – Karen Harvey Prize, Alexis Rouillard: Probing the Origin of Slow SolarWind, Coronal Mass Ejections and Solar Energetic Particles by CombiningSolar and Heliospheric Imagery with In-situ MeasurementsPlenary Session – America Ballroom North/Central – 03 Jun 2014 03:40 PM to 04:30 PMChair(s):Leon Golub (SAO)

216.01 – Probing the origin of slow solarwind, coronal mass ejections and solarenergetic particles by combining solar andheliospheric imagery with in-situmeasurements.The Solar-Terrestrial Relations Observatory (STEREO),launched in 2006, is equipped with cameras that areobserving the Sun and heliosphere from two vantagepoints. The orbital configuration of the spacecraft changedrapidly during the course of the current solar cyclepermitting a wide range of different studies to be carriedout on various timescales. Combined STEREO observationshave provided new insights on the origin of the variable

slow solar wind, the global topology of CMEs and theirshocks and the origin of high-energy solar energeticparticles. We will review these recent discoveries and thenfocus on a series of analyses that combine ultraviolet andwhite-light images to track in 3-D the spatial and temporalevolution of coronal pressure waves associated with theonset of CMEs. We will then combine coronal imagery ofthese shocks with in-situ measurements of solar energeticparticle events (SEPs) to study the acceleration andpropagation mechanisms of high-energy particles in thesolar corona.Author(s): Alexis Rouillard (Universite de Toulouse)

217 – Margaret Meixner: The Life Cycle of Dust in the Magellanic Clouds:Insights from Spitzer and HerschelPlenary Session – America Ballroom North/Central – 03 Jun 2014 04:30 PM to 05:20 PMChair(s):Edward Churchwell (Univ. of Wisconsin)

217.01 – The Life Cycle of Dust in theMagellanic Clouds: Insights from Spitzerand HerschelThe life cycle of dust in a galaxy involves the exchange ofmaterial between the interstellar medium (ISM) and stars.Dust is formed in the winds of dying stars, such asasymptotic giant branch (AGB) and red supergiant (RSG)stars, and the explosion of supernovae. In the ISM, the dustmay be shattered and vaporized by supernova blast wavesor accreted onto seed grains in the denser ISM. Dust isconsumed in the star formation process and appears in thecircumstellar environments of newly forming stars. Bytracing the lifecycle of dust, we gain insights into the dustevolution processes and the origin of galactic dust. TheSpitzer Space Telescope and Herschel Space Observatoryprovide a sensitive probe of circumstellar and interstellardust. The Spitzer Surveying the Agents of Galaxy Evolution(SAGE; the ISM and stars) and the Herschel Inventory of theAgents of Galaxy Evolution (HERITAGE) surveys of the LargeMagellanic Cloud (LMC) and Small Magellanic Cloud (SMC)focus on the lifecycle of dust. The LMC and SMC are ideal

astrophysical laboratories for this study because theirproximity to us permits detailed studies of the stars andtheir relation to the ISM from local to galaxy wide scales.For example, the masses of the circumstellar dust shells ofstars and ISM dust clouds can be determined producing amore precise dust budget than possible for our own MilkyWay galaxy. I will present key results from the SAGE andHERITAGE projects that quantify the stellar origin of dust,its evolution in the ISM and its consumption by starformation. Our measurements of dust mass-loss rates fromentire populations of AGB and RSG stars and the discoveryof ~0.5 solar masses of dust in the ejecta of supernova,SN1987A, provide the dust production rates by the stars.The maps of dust masses and gas-to-dust ratios of the ISMreveal how dust is destroyed and possibly created in theISM. Our discovery of thousands of young stellar objectcandidates shows us locations of active star formation andenables us to quantify the star formation rate. I will endwith a brief summary of the potential of the James WebbSpace Telescope to extend this research.Author(s): Margaret Meixner (Johns Hopkins University)

Contributing teams: SAGE, HERITAGE

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300 – Rosanne DiStefano: New Opportunities in Gravitational Microlensingand MesolensingPlenary Session – America Ballroom North/Central – 04 Jun 2014 08:30 AM to 09:20 AMChair(s):Chryssa Kouveliotou (NASA/MSFC)

300.01 – NEW OPPORTUNITIES INGRAVITATIONAL MICROLENSING ANDMESOLENSINGIt took more than fifty years and the development ofcomputer technology to transform Einstein's theoreticalwork on what we now call "gravitational microlensing" intoan active and successful field of observational research.The first microlensing events were announced in 1993, andtoday's monitoring teams discover roughly 2000 candidateevents each year. Binaries and planets have beendiscovered, and the masses of nearby stars and browndwarfs have been measured. The total numbers of planetsdiscovered through lensing is still small, but the field isyoung, and new methods and techniques are beingdeveloped. I will summarize the successes to date, and willthen focus on some intriguing new opportunities. One ofthese opportunities is suggested by theoretical work that

will allow observers to search for planets in a wider rangeof orbits, thereby increasing the discovery rate. Anotheropportunity is provided by counterpart searches andparallax signatures in the lensing light curves, which arehelping us to identify those events caused by nearby lenses(mesolenses), located within about a kiloparsec. We canlearn a great deal more about mesolenses, and thereforeexpect to systematically discover and measure masses ofnearby brown dwarfs, neutron stars and black holes, andalso to find nearby planets that can be be studied withother techniques as well. Finally, mesolensing events canbe predicted in advance, providing a new avenue tomeasure the masses and multiplicity of nearby stars.Gravitational lensing events have a rich potential tocontribute to astronomy, and we are presently exploringnew possibilities and establishing the framework that willallow more of this potential to be realized.Author(s): Rosanne Di Stefano (Harvard-Smithsonian CfA)

– LAD Posters WednesdayPoster Session – Essex Ballroom and America Foyer – 04 Jun 2014 09:00 AM to 06:30 PM

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318 – Structure of the Early Universe PostersPoster Session – Essex Ballroom and America Foyer – 04 Jun 2014 09:00 AM to 06:30 PM

318.01 – HERA: Illuminating Our EarlyUniverseThe Hydrogen Epoch of Reionization Arrays (HERA)roadmap is a staged plan for using the unique properties ofthe 21cm line from neutral hydrogen to probe our cosmicdawn, from the birth of the first stars and black holes,through the full reionization of the primordial intergalacticmedium (IGM). HERA is a collaboration between thePrecision Array Probing the Epoch of Reionization (PAPER),US-Murchison Widefield Array (MWA), and MIT Epoch ofReionization (MITEOR) teams. The first phase of the HERAroadmap entailed the operation of the PAPER and MWAtelescopes to explore techniques and designs required todetect the primordial HI signal in the presence of radiocontinuum foreground emission some four orders ofmagnitude brighter. Studies with PAPER and the MWA haveled to a new understanding of the interplay of foregroundand instrumental systematics in the context of a three-dimensional cosmological intensity-mapping experiment.We are now able to remove foregrounds to the limits of oursensitivity with these instruments, culminating in the firstphysically meaningful upper limits on the power spectrumof 21~cm emission from reionization. Building on thisunderstanding, the next stage of HERA entails a new 14mdiameter antenna element that is optimized both forsensitivity and for minimizing foreground systematics.Arranging these elements in a compact hexagonal gridyields an array that facilitates calibration, leverages provenforeground removal techniques, and is scalable to largecollecting areas. The HERA phase II will be located in theradio quiet environment of the SKA site in Karoo, SouthAfrica, and have a sensitivity close to two orders ofmagnitude better than PAPER and the MWA, with broaderfrequency coverage, HERA can paint an uninterruptedpicture through reionization, back to the end of the DarkAges. This paper will present a summary of the currentunderstanding of the signal characteristics andmeasurements and describe this planned HERA telescopeto be built to detect and characterize the EoR powerspectrum.Author(s): David DeBoer (University of California)

Contributing teams: HERA Collaboration

318.02 – Polarization Results from PAPEREpoch of Reionization (EoR) experiments seeking adetection of the power spectrum face daunting challengesin the form of extremely bright foregrounds. One of theleast well-characterized is that of polarization emission atmeter wavelengths, both from our own Galaxy and fromextragalactic radio sources. Faraday rotation of polarizedsources produces frequency structure in the observedspectrum, and leakage of the polarized emission intoestimates of Stokes I can be confused with the fluctuationsdue to reionization. Here we present recent results oncharacterizing the power spectrum of polarized emissionthe Precision Array for Probing the Epoch of Reionization(PAPER). PAPER is a focused experiment aimed at detectingthe spatial power spectrum of neutral hydrogen emissionduring the EoR. PAPER is an interferometer operating from100 - 200 MHz, with antennas measuring linear polarizationand a correlator producing full-Stokes output. The sciencearray is located at the site of the future Square KilometreArray (SKA) site in South Africa, with a prototyping and testfacility in Green Bank, WV. A staged build-out of PAPERSouth Africa (PSA) began in late 2009. PAPER has beenobtaining science-grade observations since late 2011, when32 dipoles (PSA-32) began taking data full-Stokes data, andis currently at its final size with 128 dipoles taking datasince November 2013. We present power spectrum andimaging data from PSA-32 quantifying the brightness offoreground emission. We consider lessons learned from thisexperience in the design of the Hydrogen Epoch ofReionization Array.Author(s): James Aguirre (University of Pennsylvania)

Contributing teams: PAPER Collaboration, HERACollaboration

318.03 – Epoch of Reionization PowerSpectrum Measurements from PAPER toHERAIn the next few years, low-frequency radio interferometerarrays will achieve a first detection of the highly redshifted21cm line of neutral hydrogen. These measurements willact as the first direct probe of the IGM between redshifts 20and 6, enabling a new understanding of the physicalprocesses at play during Cosmic Dawn and the Epoch ofReionization. We present upper limits on the 21cm powerspectrum at z = 7.7 from the Precision Array for Probing theEpoch of Reionzation (PAPER), a current-generationinstrument, as well as forecasts for the Hydrogen Epoch ofReionization Array (HERA), a planned next-generationexperiment. We also discuss the tight constraints that HERAwill place on astrophysical parameters pertaining to thefirst luminous objects (such as their ionizing efficiency) andthe environments in which they form. Finally, we illustratehow systematics such as foreground emission can beovercome.Author(s): Adrian Liu (University of California Berkeley), JonathanPober (University of California Berkeley), Joshua Dillon (MassachusettsInstitute of Technology), Aaron Parsons (University of California Berkeley)

Contributing teams: HERA collaboration

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318.04 – Power Spectrum Estimation for 21cm CosmologyTomography with the 21 cm line of neutral hydrogenpresents the opportunity to directly probe a vast fraction ofthe comoving volume of the observable universe at timeswhen more established techniques are unavailable. Thepower spectrum of 21 cm brightness temperaturefluctuations from the Epoch of Reionization and precedingeras will likely be the first key measurement for comparingtheory and observation and constraining models ofastrophysics and cosmology during the Cosmic Dawn. Inthis poster, I will present the statistical and algorithmicchallenges presented by making this measurement in thepresence of foregrounds that are orders of magnitudestronger than the signal. I will also show progress that hasbeen made to overcome these challenges with data fromthe Murchinson Widefield Array and the implication forfuture experiments and analysis techniques.Author(s): Joshua Dillon (Massachusetts Institute of Technology)

318.05 – Constraining the population ofradio-loud active galactic nuclei at highredshift with the power spectrum of the 21cm ForestThe 21 cm forest, the absorption by the intergalacticmedium (IGM) towards a high redshift radio-loud source, isa probe of the thermal state of the IGM. To date, theliterature has focused on line-of-sight spectral studies of asingle quasar known to have a large redshift. We insteadexamine many sources in a wide field of view, and showthat the imprint from the 21 cm forest absorption of thesesources is detectible in the power spectrum. The propertiesof the power spectrum can reveal information on thepopulation of the earliest radio loud sources that may haveexisted during the pre-reionization epoch at z>10. Usingsemi-numerical simulations of the IGM and a semi-empiricalsource population, we show that the 21 cm forestdominates, in a distinctive region of Fourier space, thebrightness temperature power spectrum that manycontemporary experiments aim to measure. In particular,the forest dominates the diffuse emission on smaller spatialscales along the line of sight. Exploiting this separation,one may constrain the IGM thermal history, such as heatingby the first X-ray sources, on large spatial scales and theabsorption of radio loud active galactic nuclei on smallones. Using realistic simulations of noise and foregrounds,we show that planned instruments on the scale of theHydrogen Epoch of Reionization Array (HERA) with acollecting area of one tenth of a square kilometer candetect the 21cm forest in this small spatial scale regionwith high signal to noise. We develop an analytic toy modelfor the signal and explore its detectability over a largerange of thermal histories and potential high redshiftsource scenarios.Author(s): Aaron Ewall-Wice (MIT), Joshua Dillon (MIT), AndreiMesinger (Scuola Normale Superiore), Jacqueline Hewitt (MIT)

318.06 – Measuring antenna tilebeampatterns with high dynamic range forthe Murchison Widefield Array using 137MHz ORBCOMM satellitesDetection of the redshifted 21cm fluctuations from theEpoch of Reionization in thousand hour integrations posesstringent requirements on calibration and image quality,both of which necessitate accurate primary beam models.The Murchison Widefield Array (MWA) uses phased arrayantenna elements designed to maximize collecting area atthe expense of modeling complexity. To quantify theirperformance, we have developed a novel beammeasurement system using the 137 MHz ORBCOMMsatellite constellation and a reference dipole antenna.Using power ratio measurements, we measure the in siturelative beampattern of the MWA antenna tile, evadingvariation of satellite flux or polarization with time. Weemploy angular averaging to mitigate multipath effects(ground scattering), and assess environmental systematicswith a "null experiment” in which the MWA tile is replacedwith a second reference dipole. We achieve beammeasurements with 30 dB dynamic range over a large fieldof view, far wider and deeper than drift scans throughastronomical sources allow. We verify an analytic model forthe MWA tile within few percent statistical scatter in themain lobe. Towards the edges of the main lobe and in thesidelobes, we measure tens of percent systematicdeviations, in rough agreement with modeled beamformingerrors. We discuss requirements for possible futurecalibration systems deployed on unmanned aerial vehiclesor low Earth orbit satellites.Author(s): Abraham Neben (MIT Kavli Institute for Astrophysicsand Space Research), Richard Bradley (National Radio AstronomyObservatory), Jacqueline Hewitt (MIT Kavli Institute for Astrophysics andSpace Research)

318.07 – MITEoR: scalable interferometertechnology for precision cosmologyWe describe the instrument design and calibration resultsof MITEoR, a path-finder 21 cm interferometer focusing onprecision calibration and scalability. 21 cm cosmology is agrowing field aiming to probe a large and previouslyinaccessible volume of our high redshift universe. However,the resulting constraints on cosmological parameters willonly be as good as the instrumental calibration. We havesuccessfully demonstrated several novel and scalableprecision calibration techniques, which can help nextgeneration experiments like HERA achieve unprecedentedprecision in 21 cm measurements.Author(s): Haoxuan Zheng (MIT)

Contributing teams: MITEoR

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318.08 – The HI Mass Function and VelocityWidth Function of Void Galaxies in theArecibo Legacy Fast ALFA SurveyWe measure the HI mass function (HIMF) and velocity widthfunction (WF) across environments over a range of massesand profile widths using a catalog of ~7,300 HI-selectedgalaxies from the ALFALFA Survey, located in the region ofsky where ALFALFA and SDSS (Data Release 7) Northoverlap. We divide our galaxy sample into those that residein large-scale voids (void galaxies) and those that live indenser regions (wall galaxies). We find the void and wallHIMFs are well fit by Schechter functions. We conclude thatvoid galaxies typically have lower HI masses than theirnon-void counterparts, which is in agreement with the darkmatter halo mass function shift in voids; and the voidlow-mass slope is shallower than that of the wall HIMFsuggesting that there is either no excess of low-massgalaxies in voids or there is an abundance of intermediateHI mass galaxies. We fit a modified Schechter function toboth the ALFALFA void and wall WFs. Because of largeuncertainties on the void and wall WFs, we cannot concludewhether these functions are dependent on environment.Author(s): Crystal Moorman (Drexel University), Michael Vogeley(Drexel University), Fiona Hoyle (Pontifica Universidad Catolica deEcuador), Danny Pan (Shanghai Astronomical Observatory), MarthaHaynes (Cornell University), Riccardo Giovanelli (Cornell University)

318.09 – Galactic Extinction, CepheidDistances, and the Hubble ConstantGalactic interstellar extinction is tested using reddeningline parameters for several Galactic plane fields inconjunction with reddening slope X = E(U-B)/E(B-V) valuesand stellar equivalent widths W(?4430). The extinctionparameter RV(observed}) displays a quadratic variationwith reddening slope X, with a minimum at RV = 2.82±0.06for X = 0.83. ?4430 absorption also displays a dependenceon reddening slope, with no absorption for stars with X =0.83, increasing with decreasing X, and saturating nearX=0.75. Galactic extinction therefore appears to follow a

relation described by A(?) ? ?-1.375, which differs in severalrespects from generally adopted laws but matchesexpectations from Zagury (2013) for forward scattering ofstarlight by hydrogen in the Galactic plane. Extinctiontowards other galaxies should therefore be similar to that inregions where X = 0.83 and RV = 2.82, implying slightlyunderestimated distances to extragalactic Cepheids. Areworking of data for Cepheids in the megamaser galaxyM106 using a Wesenheit formulation of the PL relation withRV = 3 (appropriate for Cepheids) rather than 3.3 yields: (i)reasonably close agreement of the galaxy’s distance fromCepheids both close to and distant from the galactic core,(ii) a new estimate of 7.98±0.41 Mpc for the distance to thegalaxy, and (iii) implied values for the Hubble constant ofH0 = 61.7±3.2 km/s/Mpc for the motion of M106 relative toa Milky Way/LMC barycenter of the Local Group, or H0 =64.7±3.4 km/s/Mpc if infall of M106 towards the Virgocluster is included. The corresponding values relative to aMilky Way/M31 barycenter are 63.6±3.3 km/s/Mpc and66.6±3.4 km/s/Mpc, respectively. Differences with respectto previously published values emphasize the importanceof reddening corrections and Local Group dynamics in usingCepheids to establish the local rate of expansion of theUniverse.Author(s): David Turner (Saint Mary's Univ.)

318.10 – Identifying a Damped Lyman AlphaSource in the Spectrum of Quasar SDSSJ233544.18+150118.3We present the nebular properties of a DLA along theline-of-sight of the quasar SDSS J233544.18+150118.3. Weobtained two IFU spectra with UH 2.2m/SNIFSapproximately 4 arcseconds south of the quasar. A carefulanalysis of the sky spectra surrounding the DLA thenallowed us to generate a high SNR sky spectrum. Through aclose examination of our reduced images, we havesuccessfully identified a faint but distinct source of [OII]emission at the same redshift reported elsewhere for thedamped Lyman-Alpha absorption lines in the quasar'sspectrum. Further investigation also revealed the presenceof lower intensity H-beta emission lines at the sameredshift. Based on the relative intensities of the [OII] andH-beta lines in the spectrum of this relatively dimintervening galaxy, we present some initial conclusionsregarding nebular abundance and star formation rate inthis newly identified galaxy, and how its propertiescompare with a representative sample of galaxies at similarredshifts and luminosities.Author(s): Benjamin Browning (Department of Physics andAstronomy, University of Hawaii at Hilo), Marianne Takamiya(Department of Physics and Astronomy, University of Hawaii at Hilo), MarkChun (Institute for Astronomy, University of Hawaii at Manoa), VarshaKulkarni (Department of Physics and Astronomy, University of SouthCarolina), Soheila Gharanfoli (Department of Physics and Astronomy,University of South Carolina)

318.11 – Environmental factors affectingGalaxy Morphology - a study using COSMOSAccording to our current understanding, galaxy shapes andmorphologies should depend on various factors such as thelocal environment. Realistic image simulations forcalibration of weak lensing analysis methods that usetraining samples from the Hubble Space Telescope cantherefore be affected by these trends, due to the limitedvolume of the universe that has been surveyed by Hubble. Iwill show how redshift slices in a volume-limited subsampleof COSMOS can be classified as overdense or underdense(or neither), and how the statistical properties of variousmorphological parameters such as ellipticity, Sersic n,bulge-to-total ratio and color differ in these bins. This studyrequires a careful distinction between environment effectsfrom large-scale structure, which we do not wish to includein simulations, and general trends in the galaxy populationwith redshift. We conclude with some guidance for howupcoming surveys can use COSMOS data as the basis forweak lensing simulations without having their conclusionsoverly affected by cosmic variance.Author(s): Arun Jayaraman (Carnegie Mellon University), RachelMandelbaum (Carnegie Mellon University), Claire Lackner (Kavli Institutefor the Physics and Mathematics of the Universe (WPI), Todai Institutes forAdvanced Study, the University of Tokyo)

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318.12 – Effects of Multiple WeakDeflections on the Galaxy-Galaxy LensingSignalGalaxy-galaxy lensing is a powerful tool with which the darkmass distribution around galaxies can be constraineddirectly. One potential complication to the interpretation ofan observed galaxy-galaxy lensing signal, however, is theeffect of multiple weak deflections. A number of previousstudies have shown that for a typical deep data set,background source galaxies will have been lensed at acomparable level by two or more foreground galaxies.Contrary to naive expectations, these multiple weakdeflections that are undergone by the images of the sourcegalaxies do not generally cancel out, nor can they usuallybe ignored. Previous work as shown that at large angularscales the net shear experienced by distant source galaxiesdue to all foreground lenses generally exceeds the sheardue to the single lens with the smallest impact parameter(the "closest lens"). When multiple deflections that haveoccurred in the observational data are not included in theinterpretation of the observed shear profile, systematicerrors in the constraints on the lens masses can occur. Herewe explore the effects of multiple deflections on the galaxy-galaxy lensing signal using various toy models. We showthat the main cause for the difference between the shearprofile resulting from all foreground weak lenses and theshear profile resulting from the single closest weak lens isthe fact that galaxies have a broad distribution in redshiftspace. That is, it is not correct to consider realistic galaxy-galaxy lensing as being confined primarily to a single lensplane in redshift space. We also explore the effect of

multiple weak deflections on the surface mass densityinferred for foreground lenses when the net meantangential shear (i.e., the shear that results when allmultiple weak deflections are taken into account) is used.Author(s): Tereasa Brainerd (Boston Univ.), Kelly Blumenthal (BostonUniv.)

318.13 – Detectability of Radio Afterglowsfrom Compact Binary CoalescenceElectromagnetic (EM) follow-up of gravitational wave (GW)candidates are both important and valuable for theverification of their astrophysical nature and the study oftheir physical properties. While the next generation of GWdetectors will have improved sensitivities expected to makethe first detection of GW events, their ability to localizethese events on the sky will remain poor during the earlyphases of operation. This makes EM follow-up challengingfor most telescopes. Many new low frequency radiotelescopes have recently come online or will come onlineover the next few years, and their wide fields of view allowthem to cover large areas of the sky in a short time. Here,we study the detectability of radio afterglows from compactbinary coalescence, a predicted GW source and the mostpromising progenitor of short gamma-ray bursts (SGRB).We explore the properties of simulated SGRB afterglowlightcurves for a range of energies, densities, observingangles and frequencies, then we use these lightcurves toestimate the expected rates of detection for different lowfrequency radio instruments and survey methods. Most ofthese instruments will be able to detect SGRB afterglows orconstrain the rates of compact binary coalescence.Author(s): Lu Feng (MIT), Ruslan Vaulin (MIT), Jacqueline Hewitt (MIT)

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319 – Surveys and Large Programs PostersPoster Session – Essex Ballroom and America Foyer – 04 Jun 2014 09:00 AM to 06:30 PM

319.01 – The Blanco DECam Bulge Survey(BDBS): Current status and progressWe present a progress update on a large multi-epochphotometric survey we have undertaken with DECamtowards the Southern Bulge of the Milky Way galaxy andalso the Sgr dwarf spheroidal galaxy. Our survey hassufficient depth to reach below the main sequence turn-offin SDSS ugrizY filters for just over 200 square degrees overthe Southern Bulge (i.e. (-10 < l < +10 and -13 < b < -2).While we easily detect the bulge main sequence turn-off insingle image-pairs despite the high degree of crowding,initial analysis suggests we are also achieving sufficientastrometric repeatability to enable useful kinematicinvestigations through proper motions. This communicationfocuses on results and techniques from our campaign in2013A (NOAO program N0529-2013A, P.I. Rich), whichcovers the inner 10x8 degrees of the bulge as well as a4-degree wide strip along the Bulge minor axis down to b =-13 degrees. Our survey is thus already laying down theearly epochs for future proper motion-enabled LSST studiesof the galactic plane, and will provide hard data on thelikely performance of LSST towards the Bulge - and thushow to optimize planned Galactic Plane science with LSST.The lessons of our campaign for existing and future large-telescope photometric surveys of the plane will bediscussed.Author(s): William Clarkson (University of Michigan-Dearborn),Robert Rich (University of California, Los Angeles), Christian Johnson(Harvard-Smithsonian Center for Astrophysics), Andrea Kunder(Astronomisches Institut Potsdam), Scott Michael (Indiana University,Bloomington), Michael Young (Indiana University, Bloomington), CatherinePilachowski (Indiana University, Bloomington), Zachary Belanger(University of Michigan-Dearborn), Elizabeth Clyne (University of Michigan-Dearborn), Zeljko Ivezic (Astronomy Department, University ofWashington), Rodrigo Ibata (Strasbourg Observatory), Michael Irwin(Institute of Astronomy), Roberto de Propris (Cerro Tololo Inter-AmericanObseratory), Andreas Koch (Zentrum fur Astronomie, University ofHeidelberg), Annie Robin (Besancon Observatory), Mario Soto (SpaceTelescope Science Institute), Katherina Vivas (Centro de Investigaciones deAstrobnomia (CIDA))

319.02 – The Blanco DECam Bulge Survey(BDBS): Pushing to highly crowded fieldswith an LSST-like imagerWe are using DECam to undertake a large, multi-cyclephotometric survey of the Southern Milky Way Bulge andthe core of the Sgr dwarf spheroidal galaxy, with sufficientdepth to reach below the main sequence turn-off in SDSSugrizY filters for just over 200 square degrees over theSouthern Bulge (i.e. (-10 < l < +10 and -13 < b < -2). Thehigh degree of crowding towards the Bulge puts our projectin a different region of parameter-space to that of the mainDark Energy Survey (DES), and thus our reduction andanalysis methods differ in some aspects from the mainprogram (for example, in a number of our fields the DEScommunity pipeline produced erroneous astrometricsolutions, or failed to converge altogether). We presenthere our efforts and methods to push our photometry asdeep as possible in these highly crowded fields, includingestimates of measurement error and completeness. AsLSST will also be seeing-limited, our faint limits are likely tobe similar to those encountered by LSST galactic-planeobservations.Author(s): Zachary Belanger (University of Michigan-Dearborn),William Clarkson (University of Michigan-Dearborn), Robert Rich (UCLA),Christian Johnson (Harvard-Smithsonian Center for Astrophysics), AndreaKunder (Astronomsche Institut Potsdam), Scott Michael (Indiana University,Bloomington), Michael Young (Indiana University, Bloomington), CatherinePilachowski (Indiana University, Bloomington)

319.03 – SURVEYING BAADE'S WINDOW FORPOSSIBLE X-RAY COUNTERPARTS TOGRAVITATIONAL LENSING EVENTS ANDOTHER OPTICAL VARIABLESWe present the first results from our Chandra HRC-Iintermediate-depth survey of a ~1.5 square degree area inBaade's Window. Over the past ~20 years, this area of thesky has been extensively monitored by both the MOA andOGLE microlensing monitoring teams. It includes ~8500stars in the OGLE-III variable star catalog and ~800microlensing events. We will present a preliminary list ofx-ray sources brighter than ~0.5-1E-14 erg/cm^2/s, andreport on the current status of our search for opticalcounterparts from catalogs of both optical variables andlensing events.Author(s): Francis Primini (Harvard-Smithsonian, CfA), Rosanne DiStefano (Harvard-Smithsonian, CfA), Sebastien Lepine (Georgia StateUniversity), Ling Zhu (MPIA), Jifeng Liu (Eureka Scientific), Jochen Greiner(MPE), Takahiro Sumi (Osaka University), Andrzej Udalski (WarsawUniversity Observatory)

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319.04 – Establishing a Network of NextGeneration SED Standards with DA WhiteDwarfsPhotometric calibration systematic uncertainties are thedominant source of error in current type Ia supernova darkenergy studies, as well as other forefront cosmology efforts,e.g. photo-redshift determinations for weak lensing masstomography. Current and next-generation ground-basedall-sky surveys require a network of calibration stars that 1)have known spectral energy distributions (SEDs) to properlyand unambiguously account for differences in as-builtfilters, and 2) are on a common photometric zero-pointscale. We exploit the well understood SEDs of DA whitedwarf stars to establish a network of faint equatorialprimary spectrophotometric standards. We present themeasurements and analysis of 9 hot DA white dwarfs near18th mag. The analysis of high S/N spectra from Geminiyields Teff and log(g), which in turn delivers the model SEDsfrom their pure hydrogen atmospheres. These model SEDsare compared against pan-chromatic photometry from HSTWFC3 imaging to determine their reddening, and toestablish their absolute flux scales without hindrance fromthe terrestrial atmosphere. This network of stars willdirectly calibrate and cross-validate the data products ofcurrent and future surveys. This precision photometricheritage from HST will benefit existing and upcomingsurvey projects (such as DES, Pan-STARRS and LSST), anddirectly addresses one of the current barriers tounderstanding the nature of dark energy.Author(s): Abhijit Saha (NOAO), Gautham Narayan (HarvardUniversity), Thomas Matheson (NOAO), Jay Holberg (University of Arizona),Christopher Stubbs (Harvard University), Susana Deustua (STSci), RalphBohlin (STSci), Edward Olszewski (University of Arizona), Ronald Gilliland(STSci), Tim Axelrod (University of Arizona), Armin Rest (STSci)

319.05 – A deep X-ray view of the SmallMagellanic CloudWe present the first results from the Chandra Deep Surveyof the Small Magellanic Cloud (SMC). This project aims toidentify the nature of X-ray sources detected in the 1.1 MsChandra survey of the SMC, down to a detection thresholdof a few times 10^32 erg/s, in 11 fields representing young(10-100 Myr) stellar populations of different ages. We willobtain the deepest X-ray luminosity functions (XLF) forX-ray binaries (XRBs) in a star-forming galaxy. The mainscientific driver behind these observations is to study howaccreting XRBs form and evolve. We will be able to provideobservational constraints on their mass-transfermechanisms and the physical properties of the differentXRB types in the low-metallicity (Z~0.2Z?) environment ofthe SMC. We detect 50 to 90 X-ray sources in each field andmeasure the X-ray photometric and spectroscopicparameters for each of them. Analysis of their light-curvesis used to identify accreting pulsars and flaring objects. Theinitial X-ray source lists have been cross-correlated withcomprehensive optical and IR photometric andspectroscopic catalogs (such as OGLE and SAGE) todetermine the most likely optical counterparts. Based onthe combination of their X-ray and optical/IR properties, weidentify candidate Be-XRBs and interlopers such asforeground stars and AGN. We study the population ofhigh-mass XRBs, their clustering with star-forming regionsand OB associations, and the long-term variability ofidentified sources based on a comparison with previousshallow surveys of the SMC by XMM-Newton and Chandra.Author(s): Vallia Antoniou (Smithsonian AstrophysicalObservatory), Andreas Zezas (Smithsonian Astrophysical Observatory),Jeremy Drake (Smithsonian Astrophysical Observatory), Paul Plucinsky(Smithsonian Astrophysical Observatory)

Contributing teams: SMC XVP Collaboration

319.06 – Legacy ExtraGalactic UV Survey(LEGUS): Revolutionary UV astronomyThe Treasury program LEGUS (HST/GO-13364) is a154-orbit Hubble Space Telescope survey that is obtainingHST/WFC3 and HST/ACS NUV, U, B, V, and I-band imagingof 50 star-forming galaxies at distances of 4-12 Mpc. TheLEGUS targets have been carefully selected to uniformlysample a full range of global galaxy properties such asmorphology, star formation rate, mass, metallicity, internalstructure, and interaction state. We provide a first taste ofthe type and quality of the data products that will be madeavailable to the community through the websitelegus.stsci.edu. The data includes: state of the artscience-ready mosaics in five wavelengths; band-mergedcatalogs of stellar sources (including location andphotometry), band-merged catalogs of star clusters(locations, photometry, aperture corrections), catalogs ofstar cluster properties (ages, masses, extinction). andancillary data available for this galaxy sample such asGALEX, Spitzer and WISE imaging. The above catalogs willenable a wide range of scientific applications, includingcolor-magnitude diagrams and color-color diagrams of bothstars and clusters, to derive star formation histories, clusterformation histories, the evolution of stars/association/cluster clustering, and the dependence of these on galacticenvironment. These are only a few of the potentialapplications enabled by a diverse sample like LEGUS.Author(s): Leonardo Ubeda (Space Telescope Science Institute)

Contributing teams: LEGUS

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319.07 – First Results from the SpitzerExploration Program Spitzer-CANDELSIn this contribution, we introduce the Spitzer-CosmicAssembly Near-infrared Deep Extragalactic Legacy Survey(S-CANDELS), a Cycle 8 Spitzer Exploration program.S-CANDELS has recently completed a very deep survey offive premier extragalactic survey fields: COSMOS, the EGS,the UDS, HDF-N, and ECDFS. S-CANDELS benefits fromcoextensive imaging in multiple near-infrared bands by theMulti-Cycle HST Treasury Program CANDELS. The

S-CANDELS observations reach to 27 AB mag in both bandsof warm Spitzer's Infrared Array Camera (IRAC). Here wepresent the S-CANDELS survey strategy and parameters,and describe the deepest source counts ever measured atthese wavelengths, surpassing the SEDS counts by a fullmagnitude. Finally, we touch upon the implications forsource confusion for upcoming planned and proposedmissions such as JWST and WISH.Author(s): Matthew Ashby (SAO), Giovanni Fazio (SAO), Steven Willner(SAO)

Contributing teams: the S-CANDELS Team

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320 – Education and History PostersPoster Session – Essex Ballroom and America Foyer – 04 Jun 2014 09:00 AM to 06:30 PM

320.01 – A Status Report on the AASAstronomy Ambassadors ProgramThe American Astronomical Society, in partnership with theAstronomical Society of the Pacific (ASP), has launched aseries of professional-development workshops and acommunity of practice designed to improve early-careerastronomers’ ability to communicate effectively withstudents and the public. Called AAS AstronomyAmbassadors, the program provides training and mentoringfor young astronomers, from advanced undergraduates tobeginning faculty; it also provides them access to resourcesand a network of contacts within the astronomy educationand public outreach (EPO) community. Ambassadors areprovided with a library of outreach activities and resourcematerials suitable for a range of venues and audiences. Formuch of this library we are using resources developed byorganizations such as the ASP, the Pacific Science Center,and the Center for Astronomy Education for other outreachprograms, though some resources have been created byone of us (AF) specifically for this program. After a period ofevaluation and revision, the program’s “Menu of OutreachOpportunities for Science Education” (MOOSE) is nowposted on the AAS website at http://aas.org/outreach/moose-menu-outreach-opportunities-science-education.The first two Astronomy Ambassadors workshops were heldat AAS meetings in January 2013 and January 2014; eachserved 30 young astronomers chosen from about twice thatmany applicants. Web-based follow-up activities are beingprovided through a website at the ASP designed to keepcohorts of educators trained in their programs in touch withone another. The AAS is exploring ways to fund additionalworkshops at future winter meetings; suggestions are mostwelcome. Meanwhile, the Astronomy Ambassadors trainedto date have logged more than 150 outreach events,reaching many thousands of children and adults across theU.S. and Canada.Author(s): Richard Fienberg (American Astronomical Society),Andrew Fraknoi (Foothill College), Suzanne Gurton (Astronomical Society ofthe Pacific), Anna Hurst (Astronomical Society of the Pacific), DennisSchatz (Pacific Science Center)

320.02 – New FINESSE Faculty Institutes forNASA Earth and Space Science EducationIn a systematic effort to improve the preparation of futurescience teachers, scholars coordinated by the CAPERCenter for Astronomy & Physics Education Research areproviding a series of high-quality, 2-day professionaldevelopment workshops, with year-round follow-up support,for college and university professors who prepare futurescience teachers to work with highly diverse studentpopulations. These workshops focus on reforming andrevitalizing undergraduate science teaching methodscourses and Earth and Space science content courses thatfuture teachers most often take to reflect contemporarypedagogies and data-rich problem-based learningapproaches steeped in authentic scientific inquiry, whichconsistently demonstrate effectiveness with diversestudents. Participants themselves conduct science data-richresearch projects during the institutes using highlyregarded approaches to inquiry using proven models. Inaddition, the Institute allocates significant time toillustrating best practices for working with diverse students.Moreover, participants leave with a well-formulated actionplan to reform their courses targeting future teachers toinclude more data-rich scientific inquiry lessons and to bebetter focused on improving science education for a widediversity of students. Through these workshops faculty usea backwards faded scaffolding mechanism for workinginquiry into a deeper understanding of science by usingexisting on-line data to develop and research astronomy,progressing from creating a valid and easily testablequestion, to simple data analysis, arriving at a conclusion,and finally presenting and supporting that conclusion in theclassroom. An updated schedule is available atFINESSEProgram.orgAuthor(s): Timothy Slater (CAPER Center for Astronomy & PhysicsEducation Research), Stephanie Slater (CAPER Center for Astronomy &Physics Education Research), Sunette Sophia Marshall (Toogalo College),Debra Stork (University of Wyoming), J. Richard Pomeroy (University ofCalifornia - Davis)

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320.03 – Interdisciplinary ProfessionalDevelopment: Astrolabes for MedievalistsAstronomers and astronomy educators have significantlybroadened the intended audience for their outreachactivities, from the traditional venues of public schools,libraries and planetariums to national parks, coffee houses,and concert halls. At the same time, significant attentionhas been paid to improving the quality and relevance ofprofessional development directed toward preservice andinservice science teachers. Many of our outreach andprofessional development programs have also becomeincreasingly creative in their use of interdisciplinaryconnections to astronomy, such as cultural astronomy andthe history of astronomy. This poster describes a specificexample of interdisciplinary professional developmentdirected at a different audience, humanities faculty andresearchers, through hands-on workshops on the basicastronomical background and usage of an astrolabeconducted at the International Congress on MedievalStudies at Western Michigan University in 2013 and 2014.The goal was to explain the basic astronomy behindastrolabes (as well as their cultural relevance) to medievalscholars in history, literature, and other disciplines. Theintention was to increase their comfort with manipulatingand explaining astrolabes to a basic level where they couldshare their knowledge with their own college classes. In thisway the relevance of astronomy to myriad humanendeavors could be reinforced by humanities faculty withintheir own courses.Author(s): Kristine Larsen (Central Connecticut State University)

320.04 – Boston University Pre-MajorsProgram (BU Pre-Map): Promoting Diversitythrough First-Year Undergraduate ResearchOne of largest points of attrition for underrepresentedminorities in STEM fields is the transition from high schoolto college. A report from Building Engineering and ScienceTalent (BEST) demonstrates that underrepresentedminorities begin college interested in STEM fields at ratesequal to (if nor slightly above) their representation in bothcollege and the population (25%). However, by the timethey graduate, underrepresented minorities make up only15% of STEM majors and only 9% of the STEM advanceddegrees. Most of the attrition occurs during the first year ofcollege, when large classes, a lack of mentors andchallenging courses lead many students (from allbackgrounds) to consider other majors. In 2011 I startedthe Boston University Pre-Majors Program (or BU Pre-MaP),which is modeled after the University of WashingtonPre-Majors in Astronomy Program (UW Pre-MAP), a programfor recruiting, mentoring and training underrepresented,first-year introductory astronomy students (and of which Iwas an architect). As a significant part of the Pre-MAP (orPre-MaP) model, first-year students are engaged in aresearch project with a faculty or grad-student mentor andlearn many of the skills needed to be successful in science.The BU Pre-MaP uses weekly seminars to introducestudents to BU and the college environment, discuss waysto be successful in and out of the classroom, highlights theimportance of peer mentoring and cohort building andserves as a mechanism to introduce first-year students toresearch skills. In teams of two, the Pre-MaP students select(with assistance) a research mentor and work with him/heron a original research project. In addition, Pre-MaP studentsattend several field trips including (but not limited to)viewing original science documents at the Boston PublicLibrary (including a first edition Copernicus) and anobserving run at Lowell Observatory in Arizona.Author(s): Andrew West (Boston Univ.)

320.05 – Harvard Observing Project (HOP):Undergraduate and graduate observingopportunitiesThe Harvard Observing Project (HOP) engagesundergraduate students in observational astronomy andgives graduate students extra teaching experience beyondtheir required teaching fellowships. This project offersstudents opportunities to see if they are interested inastronomy, introduces them to scientific research, andprovides an opportunity for them to interact with graduatestudents in an informal setting. Observations are madeusing the 16” Clay Telescope atop the Science Center atHarvard University in Cambridge, MA. We have observed aspart of the Pro-Am White dwarf Monitoring (PAWM) andTarget Asteroids! projects, and most recently we have beenmonitoring SN2014J in the Messier 82 galaxy (see poster byM. McIntosh).Author(s): Allyson Bieryla (Harvard Univ.), Elisabeth Newton (HarvardUniv.)

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320.06 – A Visual Galaxy ClassificationInterface and its Classroom ApplicationGalaxy morphology is an important topic in modernastronomy to understand questions concerning theevolution and formation of galaxies and their dark mattercontent. In order to engage students in exploring galaxymorphology, we developed a web-based, graphicalinterface that allows students to visually classify galaxyimages according to various morphological types. Thewebsite is designed with HTML5, JavaScript, PHP, and aMySQL database. The classification interface provideshands-on research experience and training for students andinterested clients, and allows them to contribute to studiesof galaxy morphology. We present the first results of a pilotstudy and compare the visually classified types using ourinterface with that from automated classification routines.Author(s): Stefan Kautsch (Nova Southeastern University), ChauPhung (Nova Southeastern University), Michael VanHilst (NovaSoutheastern University), Victor Castro (Nova Southeastern University)

320.07 – Shaping and Shifting Worldviews:An Analysis of What Astro 101 StudentsLearned About the Role of Science inSocietyA group of graduate and undergraduate students andresearchers with the Center for Astronomy Education (CAE)have been analyzing general education introductoryastronomy (Astro 101) students’ written responses toquestions that probe their ideas about the role andrelevance of science in our society and in their lives. At theend of the semester, students were asked severalquestions to elicit their ideas about the positive andpotential negative impacts that science has on our society'sprosperity and their quality of life. Students were asked toprovide examples and justifications for the most importantdiscoveries in science, advancements in health andmedicine and innovations in technology over the pastcentury. Students were also asked to comment on whichfacet of the course (lecture, homework, in-class writings,Think-Pair-Share questions and/or Lecture-Tutorials)contributed to changing their understanding of their worldand society.Author(s): Samantha Becker (University of Arizona), Dalton Hirst(University of Arizona), Angelica Barron-Santella (University of Arizona),Edward Prather (University of Arizona), Benjamin Mendelsohn (West ValleyCollege), Colin Wallace (University of Arizona)

320.08 – Initial Development and PilotStudy Design of Interactive LectureDemonstrations for ASTRO 101Interactive lecture demonstrations (ILDs) have repeatedlyshown to be effective tools for improving studentachievement in the context of learning physics. As a firststep toward systematic development of interactive lecturedemonstrations in ASTRO 101, the introductory astronomysurvey course, a systematic review of education research,describing educational computer simulations (ECSs) revealsthat initial development requires a targeted study of howASTRO 101 students respond to ECSs in the non-sciencemajoring undergraduate lecture setting. In this project wehave adopted the process by which ILDs were designed,pilot-tested, and successfully implemented in the context ofphysics teaching (Sokoloff & Thornton, 1997; Sokoloff &Thornton, 2004). We have designed the initial pilot-test setof ASTRO 101 ILD instructional materials relying heavily onECSs. Both an instructor’s manual and a preliminaryclassroom-ready student workbook have been developed,and we are implementing a pilot study to explore theireffectiveness in communicating scientific content, and theextent to which they might enhance students’ knowledge ofand perception about astronomy and science in general.The study design uses a pre-/post-test quasi-experimentalstudy design measuring students’ normalized gain scores,calculated as per Hake (1998) and Prather (2009), using aslightly modified version of S. Slater’s (2011) Test OfAstronomy STandards TOAST combined with otherinstruments. The results of this initial study will guide theiterative development of ASTRO 101 ILDs that are intendedto both be effective at enhancing student achievement andeasy for instructors to successfully implement.Author(s): Andria Schwortz (Quinsigamond Community College), D.French (University of Wyoming), Joseph Gutierrez (University of Wyoming),Richard Sanchez (University of Wyoming), Timothy Slater (University ofWyoming), Coty Tatge (University of Wyoming)

320.09 – Skype Me! Astronomers, Students,and Cutting-Edge ResearchA primary goal of many university science courses is topromote understanding of the process of contemporaryscientific inquiry. One powerful way to achieve this is forstudents to explore current research and then interactdirectly with the leading scientist, the feasibility of whichhas recently increased dramatically due to free online videocommunication tools. We report on a program implementedat Dartmouth College in which students connect with aguest astronomer through Skype (video chat). The Skypesession is wrapped in a larger activity where studentsexplore current research articles, interact with theastronomer, and then reflect on the experience. Thein-class Skype discussions require a small timecommitment from scientists (20-30 minutes, with little orno need for preparation) while providing students directaccess to researchers at the cutting edge of modernastronomy. We outline the procedures used to implementthese discussions, and present qualitative assessments ofstudent's understanding of the process of research, as wellas feedback from the guest astronomers.Author(s): Ryan Hickox (Dartmouth College), Adrienne Gauthier(Dartmouth College)

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320.10 – Essays in the Non-Science MajorAstrobiology CourseThe non-science major "Life in the Universe" class offersstudents many opportunities to explore topics such aswhether or not to send manned missions to Mars, whichjovian moon is a suitable candidate for harboring life, etc.Some of these topics are suited to being offered asprojects. At Joliet Junior College, Joliet, IL, we offer thisgeneral education class every semester to around 40students. We expect our students to complete three shortessays in a semester, instead of doing one or two largeprojects. The essays enable students to be engaged moredeeply with some aspects of the course than is usuallypossible in the classroom. Some of our essay topics arebased on suggestions in the textbook, others have beendeveloped by us. In this poster, we will report on the essaytopics and the attitudes of our Fall 2013 and Spring 2014students to such essays.Author(s): Noella D'Cruz (Joliet Junior College)

320.11 – Changing perceptions oneclassroom at a time: Evaluation results fromthe Solar Dynamics Observatory formalEducation and Public Outreach programsThe Solar Dynamics Observatory’s (SDO) education andpublic outreach (EPO) team has developed andimplemented a number of formal education programs forK-12 students and teachers. Programs include the Day AtGoddard field trip for high school students, SDOAmbassador in the Classroom outreach to elementaryclassrooms, and teacher support materials for solar scienceeducation. These programs have been designed to fosterstudent interest and engagement in science especiallysolar science, and increase their awareness and interest inNASA and STEM careers. Magnolia Consulting, who workedclosely with the SDO EPO team to both design asubstantive evaluation program, as well as improve theeducation programs offered, has extensively evaluatedthese programs. Evaluation findings indicate that teachershighly value the opportunities and resources provided bySDO EPO and that student impacts include increasedinterest and engagement in solar science topics andawareness of STEM careers. This presentation will be asummary of the results of the evaluation of these formaleducation programs including lessons learned that can beof value to the STEM EPO community.Author(s): Martha Wawro (NASA/GSFC), Carol Haden (MagnoliaConsulting)

320.12 – Frontier Fields: Bringing theDistant Universe into ViewThe Frontier Fields is a multi-cycle program of six deep-fieldobservations of strong-lensing galaxy clusters that will betaken in parallel with six deep “blank fields.” The three-yearlong collaborative program centers on observations fromNASA’s Great Observatories, who will team up to lookdeeper into the universe than ever before, and potentiallyuncover galaxies that are as much as 100 times fainterthan what the telescopes can typically see. Because of theunprecedented views of the universe that will be achieved,the Frontier Fields science program is ideal for informingaudiences about scientific advances and topics in STEM. Forexample, the program provides an opportunity to look backon the history of deep field observations and how theychanged (and continue to change) astronomy, whileexploring the ways astronomers approach big scienceproblems. As a result, the Space Telescope ScienceInstitute’s Office of Public Outreach has initiated aneducation and public outreach (E/PO) project to follow theprogress of the Frontier Fields program – providing abehind-the-scenes perspective of this observing initiative.This poster will highlight the goals of the Frontier FieldsE/PO project and the cost-effective approach being used tobring the program’s results to both the public andeducational audiences.Author(s): Bonnie Eisenhamer (STScI), Brandon Lawton (STScI), FrankSummers (STScI), Holly Ryer (STScI)

320.13 – Elizabeth Brown and theClassification of Sunspots in the 19thCenturyBritish amateur astronomers collected solar observationdata as members of organizations such as the BritishAstronomical Association (BAA) and Liverpool AstronomicalSociety (LAS) in the late 1800s. Amateur astronomerElizabeth Brown (1830-99) served as Solar Section Directorof both groups, and not only aggregated solar observations(including hand-drawn illustrations) from observers fromaround the globe, but worked closely with solar astronomerEdward Maunder and other professionals in an attempt togarner specific types of observations from BAA members inorder to answer a number of astronomical questions of theday. For example, she encouraged the monitoring of thegrowth and decay of sunspot groups and published anumber of her own observations of particular groups,urging observers to note whether faculae were seen beforethe birth of sunspots in a given region, a topic ofcontroversy at that time. She also developed a system forclassifying sunspots and sunspot groups based on theirappearance, dividing then into 11 types: normal,compound, pairs, clusters, trains, streams, zigzags,elliptical, vertical, nebulous, and dots. This poster willsummarize Brown’s important contributions to solarobserving in the late 19th century and situate herclassification scheme relative to those of A.L. Cortie (1901),M. Waldmeier (1938; 1947) and the modified Zurich systemof McIntosh (1966; 1969; 1989).Author(s): Kristine Larsen (Central Connecticut State University)

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321 – The Sun and The Solar System PostersPoster Session – Essex Ballroom and America Foyer – 04 Jun 2014 09:00 AM to 06:30 PM

321.02 – Forward Modeling of CoronalEmissionIn this work, we present simulations of the coronal emissionin Extreme Ultraviolet wavelengths, subject to the possiblephysical models of how the solar corona is heated. In orderto maximize the match of the simulations with theobservations, we also use models of coronal magnetic fieldwhich are constructed to match the observed coronalfeatures (see Malanushenko et al, 2014). While we utilizethe 1D quasi-steady atmosphere approach (as in Schrijver& van Ballegoijen, 2005), we take a step away from thecommonly used assumption about circular cross-sections ofmagnetic flux tubes, as our previous research(Malanushenko & Schrijver, 2013) suggests that thisassumption might lead to substantial artefacts whencomparing the simulations to the observations. In this work,we explore how such treatment of magnetic flux tubes iscapable of producing realistic coronal features. Using thesetwo major advances, the realistic field model and therealistic treatment of the cross-section of flux tubes, wetest a wide range of possible heating scenarios, ruling outpossibilities by comparing the simulations with data from awide range of EUV channels onboard SDO/AIA spacecraft.Author(s): Anna Malanushenko (Lockheed Martin AdvancedTechnology Center), Carolus Schrijver (Lockheed Martin AdvancedTechnology Center), Adriaan Van Ballegooijen (Harvard-Smithsonian Centerfor Astrophysics)

321.03 – Chandra Observations andModeling of Geocoronal Charge ExchangeX-Ray Emission During Solar Wind GustsSolar wind charge exchange (SWCX) X-rays are emittedwhen highly charged solar wind ions such as O7+ collidewith neutral gas. The best known examples of this occuraround comets, but SWCX emission also arises in theEarth's tenuous outer atmosphere and throughout theheliosphere as neutral H and He from the interstellarmedium flows into the solar system. This geocoronal andheliospheric emission comprises much of the soft X-raybackground and is seen in every X-ray observation.Geocoronal emission, although usually weaker thanheliospheric emission, arises within a few tens of Earth radiiand therefore responds much more quickly (on time scalesof less than an hour) to changes in solar wind intensity thanthe widely distributed heliospheric emission. We havestudied a dozen Chandra observations when the flux ofsolar wind protons and O7+ ions was at its highest. Thesegusts of wind cause correspondingly abrupt changes ingeocoronal SWCX X-ray emission, which may or may not beapparent in Chandra data depending on a givenobservation's line of sight through the magnetosphere. Wecompare observed changes in the X-ray background withpredictions from a fully 3D analysis of SWCX emissionbased on magnetospheric simulations using the BATS-R-USmodel.Author(s): Marc Kornbleuth (Harvard-Smithsonian Center forAstrophysics), Bradford Wargelin (Harvard-Smithsonian Center forAstrophysics), Michael Juda (Harvard-Smithsonian Center for Astrophysics)

321.04 – Monitoring of Transient LunarPhenomenaTransient Lunar Phenomena (TLP’s) are described asshort-lived changes in the brightness of areas on the faceof the Moon. TLP research is characterized by the inabilityto substantiate, reproduce, and verify findings. Our currentresearch includes the analysis of lunar images taken withtwo Santa Barbara Instrument Group (SBIG) ST8-E CCDcameras mounted on two 0.36m Celestron telescopes. Onone telescope, we are using a sodium filter, and on theother an H-alpha filter, imaging approximately one-third ofthe lunar surface. We are focusing on two regions: Hyginusand Ina. Ina is of particular interest because it showsevidence of recent activity (Schultz, P., Staid, M., Pieters, C.Nature, Volume 444, Issue 7116, pp. 184-186, 2006). Atotal of over 50,000 images have been obtained overapproximately 35 nights and visually analyzed to search forchanges. As of March, 2014, no evidence of TLPs has beenfound. We are currently developing a Matlab program to doimage analysis to detect TLPs that might not be apparentby visual inspection alone.Author(s): Timothy Barker (Wheaton College), Ryan Farber (WheatonCollege), Gary Ahrendts (Wheaton College)

321.05 – Hydrogen Abundance and Escapeat Mars: Where we are Now and Where weare GoingThe Space Telescope Imaging Spectrograph (STIS)instrument on board the Hubble Space Telescope (HST) hasbeen used to make high resolution observations ofLyman-alpha hydrogen (H) and deuterium (D) emissions ofMars in April 2001 and April 2012. These data show thealtitude profiles of emission across the martian disc, fromwhich a radiative transfer model can be applied to derivedensities and temperatures. D was also detected in the2001 spectra. The Mars Atmosphere and Volatile Evolution(MAVEN) mission is on the way to orbiting Mars and will bemaking similar measurements of Lyman-alpha emissionsfrom within the martian atmosphere. The more recentMAVEN measurements will be used in conjunction with HSTobservations to determine the hydrogen densities andtemperatures, the H escape rate, and the D/H ratio atvarious epochs. Implications for the of the variability ofplanetary hydrogen properties on planetary water loss willbe discussed.Author(s): Majd Mayyasi-Matta (Boston University), John Clarke(Boston University)

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321.06 – HST Observations of Mars andVenus Supra-thermal ThermosphericOxygenThe loss of water from Venus and Mars is an ongoing topicof study in planetary astronomy. One method forconsidering this loss is to examine the loss of volatiles,specifically hydrogen and oxygen, from the thermospheresof the two planets. One process by which oxygen atomsescape the Mars atmosphere is by a creation of asuprathermal population of oxygen from the dissociativerecombination of O2+, the dominant ion in the Mars andVenus ionospheres. On Venus, the same process occurs, butdue to the larger planetary mass the suprathermal coronahas not been observed as an escape mechanism by itself.Observations of hot oxygen in the Venus atmosphere dateback as far as 1978 (Bertaux et al.), though observationalconfirmation of the hot population of Mars was onlypublished as recently as 2011 (Feldman et al.) Re-analysisof the understanding of the Venus thermosphere has beenperformed after Venus Express results seemed to contrastto the Pioneer Venus observations (Lichtenegger et al.,2009). The observations presented in this work were takenof Mars using HST STIS and a low-resolution grating in 2007and of Venus using HST STIS and an echelle grating inNovember 2013. The UV spectroscopic observations ofresonantly-scattered sunlight from the 1304 Å oxygenemission are compared with modeled thermosphericpopulations.Comparisons are made with previous data setsand modeled populations, in order to better describe thetemporal variation of the suprathermal neutral oxygenpopulations.Author(s): Carol Carveth (Boston Univ.), John Clarke (Boston Univ.),Jean-Yves Chaufray (LATMOS - IPSL), Jean-Loup Bertaux (Boston Univ.)

321.07 – The Dynamics of Centaurs in the2:1 Mean Motion Resonance of Neptune8,026 massless test particles placed in or near the 2:1mean motion resonance of Neptune are integrated for 3Myrs subject only to the gravitational forces of a motionlessSun and the Jovian planets Jupiter, Saturn, Uranus, andNeptune. The RMVS method of integration is used. Initialinclinations and eccentricities of test particles are chosenfrom random from a range of 0 to 40 degrees for inclinationand 0 to 0.7 for eccentricity. The time each test particlespends librating in the resonance is determined. Themorphology of the semi-major axes of the test particlesover time is observed. Statistics are taken on the amount oftime test particles spend being classified as different smallobjects of the solar system such as SDOs, KBOs, Centaurs,short-period comets, main-belt asteroids and NEAs. Testparticles are removed from the simulation by colliding witha planet, approaching too close to the Sun (~0.005 AU),obtaining a hyperbolic or parabolic orbit, or by entering theOort Cloud at 1,000 AU. Common dynamical pathways thatCentaurs take to the inner solar system are sought for.Finally, case studies of interesting test particles areexamined.Author(s): Jeremy Wood (Hazard Community and TechnicalCollege)

Contributing teams: Center for Astrophysics andComputing at Melbourne, Australia

321.08 – Origin and mineralogy of olivine-dominated near-Earth AsteroidsDynamical lifetimes of near-Earth asteroids (NEAs) areshorter than the age of the Solar System thus necessitatingresupply from the Main Belt. The NEA population, becauseof its proximity, allows us to explore asteroids at asize-range not possible among asteroids further away in theMain Belt. There are very few olivine-dominated asteroids,identified as spectroscopic A-types (Bus & Binzel 2002,DeMeo et al. 2009), among the near-Earth population(Binzel et al. 2004). While a number of NEAs were labeledolivine-rich from visible wavelength data, near-infraredobservations of these objects prove the olivine-richpopulation is exceedingly rare. We identify (1951) Lick,(5261) Eureka, and a new third A-type object, (5131) 1990BG. Using a radiative transfer model (Shkuratov et al. 1999)and band parameter analysis we mineralogicallycharacterize and compare these three olivine-rich A-typeasteroids. Additionally, using the model from Bottke et al.2002, we present main-belt source regions for these bodies.Finally, we compare these NEA A-types to the main beltA-type population.Author(s): Brian Burt (Massachusetts Institute of Technology),Francesca DeMeo (Harvard-Smithsonian Center for Astrophysics), RichardBinzel (Massachusetts Institute of Technology)

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321.09 – The distribution of mantle materialamong main-belt asteroidsWe expect there to have been many bodies in the MainAsteroid Belt (MB) sufficiently heated at the time of solarsystem formation to allow their interiors to differentiate intoan iron core and silicate-rich crust and mantle. Evidence forearly solar system differentiation includes the diversity ofiron meteorites that imply the existence of over 60 distinctparent bodies (Mittlefehldt et al. 2006). Searches havebeen performed to identify silicate-rich basaltic crustmaterial (spectral V-type asteroids) in the outer MB havebeen successful (e.g., Roig et al. 2006, Masi et al. 2008,Moskovitz et al. 2008, Solontoi et al. 2012). The olivine-richmantles of differentiated asteroids should have producedsubstantially greater volumes (and therefore substantiallygreater numbers) of remnant asteroids compared withbasaltic and iron samples. Yet olivine-rich asteroids(A-types) are one of the rarest asteroid types (Bus & Binzel2002, DeMeo et al. 2009). An alternative way to search fordifferentiated bodies that have been heavily or completelydisrupted is to identify these spectral A-type asteroids,characterized by a very wide and deep 1 micron absorptionindicative of large amounts (> 80%) of olivine. Burbine etal. (1996) proposed that these asteroids are only foundamong the largest because most were “battered to bits”due to collisions, so smaller A-types were below ourdetection limit. Using the Sloan Digital Sky Survey MovingObject Catalog to select A-type asteroid candidates, wehave conducted a near-infrared spectral survey of asteroidsover 12 nights in the near-infrared in an effort to determinethe distribution and abundance of crustal and mantlematerial across the Main Asteroid Belt (MB). From threedecades of asteroid spectral observations only ~10 A-typeasteroids have been discovered. In our survey we havedetected >20 A-type asteroids thus far throughout the belt,tripling the number of known A-types. We present thesespectra and their distribution throughout the MB. Weestimate the total mass of mantle material present in thebelt today and discuss the implications.Author(s): Francesca DeMeo (Massachusetts Institute ofTechnology), Benoit Carry (Institut de Mecanique Celeste et de Calcul desEphemerides), Richard Binzel (Massachusetts Institute of Technology),Nicholas Moskovitz (Lowell Observatory), David Polishook (MassachusettsInstitute of Technology), Brian Burt (Massachusetts Institute of Technology)

321.10 – The Need for Speed:Characterizing Near Earth AsteroidsThe current discovery rate of Near Earth Asteroids (NEAs) isset to increase dramatically in the next few years from~900/year to 2,000-3,000/year thanks to new andupgraded surveys. Characterization of this population iscrucial to science, space missions, and planetary hazardassessment. Despite this, the rate of followup observationsis expected to remain the same, at ~100 spectra and a fewdozen light curves collected per year. At this rate it wouldtake up to a century to characterize just the NEA populationwith sizes above 100m. Herein we discuss the challenges ofNEA followup observations, and we show quantitatively whythese are optimally made within days of discovery. Wedescribe how a semi-dedicated 4m-class telescope cankeep better pace with projected discoveries and allow us toconstrain NEA compositions, constructions, sizes, spins, andorbits.Author(s): Kim McLeod (Wellesley College), Jose Luis Galache(Smithsonian Astrophysical Observatory), Charlie Beeson (University ofSouthampton), Martin Elvis (Smithsonian Astrophysical Observatory)

321.11 – REgolith X-Ray ImagingSpectrometer (REXIS) Aboard NASA’sOSIRIS-REx MissionThe REgolith X-Ray Imaging Spectrometer (REXIS) is astudent-led instrument being designed, built, and operatedas a collaborative effort involving MIT and Harvard. It is apart of NASA's OSIRIS-REx mission, which is scheduled forlaunch in September of 2016 for a rendezvous with, andcollection of a sample from the surface of the primitivecarbonaceous chondrite-like asteroid 101955 Bennu in2019. REXIS will determine spatial variations in elementalcomposition of Bennu's surface through solar-induced X-rayfluorescence. REXIS consists of four X-ray CCDs in thedetector plane and an X-ray mask. It is the first coded-aperture X-ray telescope in a planetary mission, whichcombines the benefit of high X-ray throughput of wide-fieldcollimation with imaging capability of a coded-mask,enabling detection of elemental surface distributions atapproximately 50-200 m scales. We present an overview ofthe REXIS instrument and the expected performance.Author(s): JaeSub Hong (Harvard Univ.), Branden Allen (HarvardUniv.), Jonathan Grindlay (Harvard Univ.), Richard Binzel (MIT), RebeccaMasterson (MIT), Niraj Inamdar (MIT), Mark Chodas (MIT), Matthew Smith(MIT), Mark Bautz (MIT), Steven Kissel (MIT), Jesus Noel Villasenor (MIT),Antonia Oprescu (Harvard Univ.)

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322 – Stars and Stellar Populations PostersPoster Session – Essex Ballroom and America Foyer – 04 Jun 2014 09:00 AM to 06:30 PM

322.01 – A Novel Tool for the SpectroscopicInference of Fundamental StellarParametersWe present a novel approach for making accurate andunbiased inferences of fundamental stellar parameters(e.g., effective temperature, surface gravity, metallicity)from spectroscopic observations, with reference to a libraryof synthetic spectra. The forward-modeling formalism wehave developed is generic (easily adaptable to data fromany instrument or covering any wavelength range) andmodular, in that it can incorporate external prior knowledgeor additional data (e.g., broadband photometry) andaccount for instrumental and non-stellar effects on thespectrum (e.g., parametric treatments of extinction, spots,etc.). An approach that employs adaptive correlated noiseis used to account for systematic discrepancies betweenthe observations and the synthetic spectral library,ensuring that issues like uncertainties in atomic ormolecular constants do not strongly bias the parameterinferences. In addition to extracting a set of unbiasedinferences of the (posterior) probability distributions forbasic stellar parameters, our modeling approach also"maps" out problematic spectral regions in the syntheticlibraries that could be used as a basis for improving themodels. As a demonstration, we present some preliminaryresults from modeling optical spectra of well-characterizedexoplanet host stars and nearby pre-main sequence stars.A basic set of adaptable software that performs thismodeling approach will be released publicly.Author(s): Ian Czekala (Harvard Smithsonian Center forAstrophysics), Sean Andrews (Harvard Smithsonian Center forAstrophysics), David Latham (Harvard Smithsonian Center forAstrophysics), Guillermo Torres (Harvard Smithsonian Center forAstrophysics)

322.02 – Probing Stellar Populations in theVirgo and Fornax Clusters with InfraredSurface Brightness FluctuationsSurface brightness fluctuations (SBF) are a useful tool formeasuring extragalactic distances. At infrared wavelengths,SBF break the age-metallicity degeneracy and are usefulfor probing the properties of the most luminous stars in agalaxy, even when individual stars are not resolved. Wepresent a detailed comparison of F110W and F160W SBFmeasurements made using the Hubble Space TelescopeWFC3/IR camera to a variety of stellar population models,including those with solar-scaled and alpha-enhancedcompositions and models incorporating convective coreovershoot for younger populations. We use these modelcomparisons to assess the star formation histories of 16galaxies spanning a wide range in color and luminosity inthe Virgo and Fornax clusters, measured as a function ofdistance from the galaxy center in elliptical apertures. Wediscuss the implications of population variations on thefluctuation magnitudes and distance measurements.Author(s): Joseph Jensen (Utah Valley University), Zachary Gibson(Utah Valley University), Hyun-chul Lee (The University of TexasPan-American), John Blakeslee (Herzberg Astrophysics)

322.03 – Coronae at 3 Gyr: First Resultsfrom a Chandra Observation of the OpenCluster Ruprecht 147Ruprecht 147 is the oldest nearby star cluster, with an ageof 3 Gyr and a distance of 300 pc. This makes it animportant benchmark in exploring activity-age-rotationrelationships, bridging the gap between the Hyades andM67. We present the first results from a deep 250 ksecACIS-I observation of the cluster. Analysis of the longest (81ksec) pointing detects more than half of the knownmembers in the field, with spectral types ranging from F6to K5. The star most like the Sun in our sample, a G2V, hasan X-ray luminosity (0.2-7 keV) of L_X ~ 1.1e28 ergs/s,which suggests a scaling with age t of log L_X ~ -b log twhere 1.25 < b < 4, possibly steeper than seen at youngerages. This research was supported by Chandra grantG02-13022X.Author(s): Steven Saar (Harvard-Smithsonian, CfA), Jason Curtis(Penn State), Jason Wright (Penn State)

322.04 – gPhoton: A Time-Tagged Databaseof Every GALEX Photon and Early ScienceResultsThe Galaxy Evolution Explorer (GALEX) mission observed alarge fraction of the sky in FUV and NUV at time resolutionsof five thousandths of a second, spanning a decade ofoperation. Due to technical limitations when the data werefirst archived, the ability to use GALEX data at such hightime resolutions was limited: the primary data productswere images that were combined into several-minuteintegrations, along with source catalogs. MAST is pleased tointroduce gPhoton, a time-tagged database of every photonevent detected by GALEX during its lifetime; some 1.5trillion events in total. This database is accompanied byboth a python-based software package and a web interface.These tools allow users to create calibrated lightcurves,intensity maps, and animated movies from any set ofphotons selected across any tile. Users can specify customapertures sizes, coordinates, and time steps down to thelevel of seconds. We present some early science cases withgPhoton, which include studies of flare stars, Be stars, andunique opportunities with objects in the Kepler field.Author(s): Scott Fleming (Space Telescope Science Institute),Chase Million (Million Concepts, Inc), Bernie Shiao (Space TelescopeScience Institute), Randy Thompson (Space Telescope Science Institute),Shui-Ay Tseng (Space Telescope Science Institute), Anthony Rogers (SpaceTelescope Science Institute), Myron Smith (NOAO), Richard White (SpaceTelescope Science Institute), Karen Levay (Space Telescope ScienceInstitute)

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322.06 – Identifying Solar Analogs in theKepler FieldSince human beings live on a planet orbiting a G2 V star, tous perhaps the most intrinsically interesting category ofstars about which planets have been discovered is solaranalogs. While Kepler has observed more than 26000targets which have effective temperatures within 100K ofthe Sun, many of these are not true solar analogs due toactivity, surface gravity, metallicity, or otherconsiderations. Here we combine ground-basedmeasurements of effective temperature and metallicitywith data on rotational periods and surface gravitiesderived from 16 quarters of Kepler observations to producea near-complete sample of solar analogs in the Kepler field.We then compare the statistical distribution of stellarphysical parameters, including activity level, for subsets ofsolar analogs consisting of KOIs and those with no detectedexoplanets. Finally, we produce a list of potential solartwins in the Kepler field.Author(s): Derek Buzasi (Florida Gulf Coast University), AndrewLezcano (Florida Gulf Coast University), Heather Preston (Florida GulfCoast University)

322.07 – Characterization of SmallExoplanet Solar-like Host Stars in theKepler FieldThis poster will discuss the stellar characteristics of over200 Kepler exoplanet host stars. The sample contains starsof V magnitude 11 to 16, spans F2 to K3 dwarfs andsubgiants, and ranges in metallicity -0.25<[Fe/H]<+0.3.These stars are solar-like in mass and radius and eachharbors at least one exoplanet of radius <2.6 R_Earth. Wedetermine the distances to the stars and find that most liewithin the thin disk of the Galaxy. Using Kepler light curvesof the sample, we examine their variability on ``transit"time scales (6-12 hr) and conclude that, to date, there is astrong bias whereby Kepler discovered small planets areonly found orbiting the photometrically quietest stars.Additionally, we show that there appears ot be norelationship between the quietest stars and their spectraltype or luminosity class and subgiants showing RV jitter canbe photometrically quiet.Author(s): Steve Howell (NASA ARC), Mark Everett (NOAO), DavidCiardi (NASA Exoplanet Inst), David Silva (NOAO), Paula Szkody (Universityof Washington)

322.08 – SOLAR ANALOGS AND TWINS SHEDA NEW LIGHT ON THE RELATION BETWEENROTATION PERIODS AND CYCLE LENGTHS OFSTELLAR ACTIVITYThe question of how typical the Sun is within the class ofsolar-type stars has been the subject of active investigationover the past three decades. Some previous work hassuggested that the Sun's magnetic cycle period Pcyc isunusual compared with similar stars, falling betweensequences of active and inactive stars. The HARPS planet-search has been gathering high-precision Ca II H&Kchromospheric activity measurements for about 7 years,and has measured a large number of new Pcyc. We collectthe most robust cycles among these for stars which aresolar analogs (main-sequence stars with 0.8 Msun < mass< 1.2 Msun) or solar twins twins (stars with Teff, [Fe/H] andmass indistinguishable from the Sun). Combining this newsample with older data, we revisit the relation betweenrotation periods Prot and Pcyc. Our preliminary analysisshows that the Sun does not has a special position betweenthe active and inactive sequences, but instead follows the anew solar-analog sequence proposed here.Author(s): José-Dias Do Nascimento (Universidade Federal do RioGrande do Norte, UFRN, Dep. de Fisica Teorica e Experimental,DFTE ), Steven Saar (Harvard-Smithsonian Center for Astrophysics),Francys Anthony (Harvard-Smithsonian Center for Astrophysics)

322.10 – WISE Infrared Excess Detectionsfor SDSS M Dwarfs: Cool Field Stars withEvidence of Warm Circumstellar MaterialWe investigate the mid-infrared properties of low-mass fielddwarfs, combining M dwarfs from the SDSS DR7spectroscopic and DR10 photometric catalogs withphotometry from the AllWISE source catalog. For thespectroscopic sample, we developed SDSS and WISEcolor-color selection criteria to select 300 M dwarfs (fromthe 70,841 in the DR7 catalog) that exhibit infrared fluxabove typical M dwarf photosphere levels at 12 and/or 22?m. We also find 30 stars within the footprint of the OrionOB1 association that have not been previously identified.Using synthetic photometry, we characterize the dustpopulations inferred from each infrared excess, and find

high fractional infrared luminosities (~10-2 L?) and orbitaldistances within the snow line (< 1 AU). Using the SDSSspectra, we measure surface gravity dependent features,and examine tracers of youth (H?, UV emission, and Liabsorption). Less than 3% of our sample shows a reliableindication of youth, implying a stellar population with ages> 1 Gyr. Our results imply that, due to the orbital distancesof our inferred dust populations and the penchant forlow-mass stars to create terrestrial planets, the most likelycause of dust in these systems is planetary collisions. Asimilar result has been used to explain the dust populationobserved around the older field star BD+20 307 (? 1 Gyr;Weinberger et al. 2011). We also present preliminaryresults using the DR10 photometric M dwarf sample. Thissample, consisting of millions of M dwarfs, allows us toexamine the phenomena of field M dwarfs exhibitinginfrared excesses in a Galactic context.Author(s): Christopher Theissen (Boston University), Andrew West(Boston University)

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322.11 – M Dwarf Stellar Activity as Noise inExoplanet DetectionA habitable-zone (HZ) planet orbiting a 0.5 solar mass Mdwarf would have a ~3 times higher likelihood of transiting,~4 times the transit depth, and a Doppler shift 3 to 4 timesstronger than the same planet orbiting in the Sun’s HZ.These factors, combined with the abundance of M dwarfs inthe galaxy—up to ~70% of stars—make M dwarfs idealtargets in the search for nearby, habitable planets.However, the high levels of magnetic activity exhibited bymany M dwarf stars, and the resulting noise introduced intoobservations, could thwart this effort. Specifically, darkspots on the stellar surface—one manifestation of stellaractivity—result in radial velocity (RV) “jitter”, which canmimic or drown out planetary signatures. In this study, wehave investigated the effects of activity-induced RV jitter onplanetary system parameters derived from RV fitting. Wemodeled the RV jitter using realistic spot models, improvingon previous jitter studies by including active latitude andlongitude ranges, evidence of which has been seen inobservations of spot distributions on low-mass stars. Weadd a planetary RV curve to the jitter data and then use anMCMC algorithm to fit RV variations and derive planetarysystem parameters. We quantify the error introduced to thederived parameters as a result of the RV jitter, focusing onplanetary period, eccentricity, and semi-major axis of orbit.We find that, on average, the measured period of theplanet is not significantly affected for filling factors of up to~10%, although higher filling factors result in derivedperiods that deviate significantly from the input period ofthe model. We show that with a zero-eccentricity model,the measured eccentricities are all non-zero and increasewith increasing spot filling-factor. Using the Kopparapu(2013) Habitable Zone estimates, we show that at highfilling factors for an M dwarf with a planet in the habitablezone, it is possible for the derived planetary orbits toscatter outside of the HZ. Our results demonstrate thatstellar RV jitter can contribute an important source of noiseto planetary measurements that must be accounted forboth when searching for and characterizing potentiallyhabitable planets around active stars.Author(s): Jan Marie Andersen (University of Copenhagen), HeidiKorhonen (University of Turku)

322.12 – Examining Flare Rates in Close MDwarf + White Dwarf Binary PairsWe present a preliminary study to examine the statisticalflare rates for M dwarfs with a close white dwarf companion(WD+dM; typical separations < 1 AU). Previous studiesshow a strong correlation between M dwarfs that are active(showing H? in emission) and their stellar flare rates. Ourprevious analysis of M dwarfs with close WD companionsdemonstrated that the M dwarfs are more active than theirfield counterparts. One implication of having a close binarycompanion is presumed to be increased stellar rotationthrough disk-disruption, tidal effects, and/or angularmomentum exchange; increased stellar rotation has longbeen attributed to an increase in stellar activity for stars.We examine the difference between the flare ratesobserved in close WD+dM binary systems and field Mdwarfs. Our sample consists of a subset of 202 (70 of whichare magnetically active) close WD+dM pairs from Morganet al. that were observed in the Sloan Digital Sky SurveyStripe 82, a transient observing mode where multi-epochobservations in the Sloan ugriz bands were obtained.Author(s): Dylan Morgan (Boston Univ.), Andrew West (Boston Univ.)

322.13 – Brown Dwarfs, DustyPhotospheres, and Surface GravityWe present new spectroscopic, photometric, andastrometric measurements of two nearby unusually dustybrown dwarfs. We show that the dusty photosphere in WISE0047+68 is due to intermediate surface gravity (betweenmost field brown dwarfs and planets) and not caused byhigh metallicity. We determine the luminosity and show thatit implies an effective temperature of ~1300K, normallytypical of T dwarfs. On the other hand, we confirm thatother red L dwarfs do not have low surface gravity.Author(s): John Gizis (Univ. Of Delaware), Katelyn Allers (Bucknell),Michael Liu (Carnegie), Jacqueline Faherty (Hawaii), Adam Burgasser (UCSan Diego), Hugh Harris (USNO)

322.14 – A Sample of Fast Moving M Dwarfsin the Milky WayIn the past decade, several high-mass stars have beendiscovered to have high enough velocities to escape theMilky Way (dubbed hypervelocity stars), yet until recently,stars with similar velocities were not observed for Solar-and lower-mass stars. There has been an observationalpaucity of hypervelocity M dwarfs, which account for ~70%of the stars in the Milky Way. While some of the shortage oflow-mass, high-velocity stars may be due to the specificmechanisms accelerating these stars, it is also possiblethat the M dwarfs have been overlooked due to their faintluminosities. We present results from a study that uses theSloan Digital Sky Survey (SDSS) Data Release 7 (DR7) MDwarf Spectroscopic Catalog (70,841 M dwarfs) to identifyand characterize several hundred M dwarfs with velocitiesgreater than 400 km/s relative to the Galactic center. Ourstudy marks the first step in demonstrating that there is asignificant sample of low-mass, high-velocity stars. Weexamined the 3D kinematics of M dwarfs in the SDSS DR7catalog with velocities > 400 km/s relative to the Galacticcenter. Stars with poor photometry or a SNR (near H-alpha)< 3 were excluded, as well as stars that were flagged in theoriginal data set as being possible M dwarf-white dwarfbinaries. We confirmed the radial velocities reported byWest et al. (2011) by manually examining the remainingstars, specifically the locations of the sodium absorptionlines (two at 5891/5897 Å, and two at 8185/8197 Å). Wepresent the final catalog of high velocity candidates and apreliminary analysis of their spectroscopically derivedproperties, including 3D kinematics, magnetic activity andmetallicity distributions.Author(s): Andrej Favia (University of Maine), Andrew West (BostonUniversity)

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322.15 – A New Sample of Cool Subdwarfsfrom SDSS: Properties and KinematicsWe present a new sample of M subdwarfs compiled fromthe 7th data release of the Sloan Digital Sky Survey. With3517 new subdwarfs, this new sample significantlyincreases the number the existing sample of low-masssubdwarfs. This catalog includes unprecedentedly largenumbers of extreme and ultra sudwarfs. Here, we presentthe catalog and the statistical analysis we perform.Subdwarf template spectra are derived. We showcolor-color and reduced proper motion diagrams of thethree metallicity classes, which are shown to separate fromthe disk dwarf population. The extreme and ultra subdwarfsare seen at larger values of reduced proper motion asexpected for more dynamically heated populations. Wedetermine 3D kinematics for all of the stars with propermotions. The color-magnitude diagrams show a clearseparation of the three metallicity classes with the ultraand extreme subdwarfs being significantly closer to themain sequence than the ordinary subdwarfs. All subdwarfslie below and to the blue of the main sequence. Based onthe average (U, V, W ) velocities and their dispersions, theextreme and ultra subdwarfs likely belong to the Galactichalo, while the ordinary subdwarfs are likely part of the oldGalactic (or thick) disk. An extensive activity analysis ofsubdwarfs is performed using chromospheric H? emissionand 208 active subdwarfs are found. We show that whilethe activity fraction of subdwarfs rises with spectral classand levels off at the latest spectral classes, consistent withthe behavior of M dwarfs, the extreme and ultra subdwarfsare basically flat.Author(s): Antonia Savcheva (Harvard-Smithsonian Center forAstrophysics), Andrew West (Boston University), John Bochanski(Haverford college)

322.16 – Period04 FCAPT uvby PhotometricStudies of Eight Magnetic CP StarsWe present Four College Automated Photometric Telescope(FCAPT) differential Stromgren uvby photometry of 8magnetic CP (mCP) stars: HD 5797 (V551 Cas), HD 26792(DH Cam), HD 27309 (56 Tau, V724 Tau), HD 49713 (V740Mon), HD 74521 (49 Cnc, BI Cnc), HD 120198 (84 UMa, CRUMa), HD 171263 (QU Ser), and HD 215441 (GL Lac,Babcock's star). Our data sets are larger than those of mostmCP stars in the literature. These are the first FCAPTobservations of HD 5797, HD 26792, HD 49713, and HD171263. Those for the remaining four stars substantiallyextend published FCAPT data. The FCAPT observed somestars for a longer time range and with greater accuracythan other optical region automated photometrictelescopes. Our goals were to determine very accurateperiods, the u, v, b, and y amplitudes, and if there were anylong period periods. In addition we wanted to compare ourresults with those of magnetic field measurements to helpinterpret the light curves. We used the Period04 computerprogram to analyze the light curves. This program provideserrors for the derived quantities as it fits the light curve.Our derived periods of 68.046 +/- 0.008 days for HD 5797,3.80205 +/- 0.00006 days for HD 26792, 1.56889 +/-0.000002 days for HD 27309, 2.13536 +/- 0.00002 days forHD 49713, 7.0505 +/- 0.0001 days for HD 74521, 1.38577+/- 0.000004 days for HD 120198, 3.9974 +/- 0.0001daysfor HD 171263, and 9.487792 +/- 0.00005 days for HD215441 are refinements of the best determinations in theliterature.Author(s): Saul Adelman (The Citadel), Robert Dukes (College ofCharleston)

322.17 – Clues to the Evolution of the RCoronae Borealis Stars from their Unique16O/18O ratiosWe report new spectroscopic observations of the CO bandsnear 2.3 micron in order to measure the 16O/18O isotopicratio in the R Coronae Borealis (RCB) stars using IRTF/SpeX.These observations of ten additional stars confirm theremarkable discovery made a few years ago that thehydrogen-deficient carbon (HdC) and RCB stars have16O/18O ratios that are close to and in some cases lessthan unity, values that are orders of magnitude smallerthan measured in other stars (the Solar value is 500). TheRCB stars are a small group of carbon-rich supergiants.Only about 100 RCB stars are known in the Galaxy. Theirdefining characteristics are hydrogen deficiency andunusual variability - RCB stars undergo massive declines ofup to 8 mag due to the formation of carbon dust at irregularintervals. The six known HdC stars are very similar to theRCB stars spectroscopically, but do not show declines or IRexcesses. Two scenarios have been proposed for the originof an RCB star: the double degenerate and the finalhelium-shell flash models. The former involves the mergerof a CO- and a He-white dwarf. In the latter, a star evolvinginto a planetary nebula central star expands to supergiantsize by a final, helium-shell flash. Greatly enhanced 18O isevident in every HdC and RCB we have measured that iscool enough to have detectable CO bands. This discovery isimportant evidence to help distinguish between theproposed evolutionary pathways of HdC and RCB stars. Nooverproduction of 18O is expected in a final flash, so we areinvestigating the merger scenario. We are working toreproduce the observed 16O/18O ratios by performinghydrodynamical simulations of the merger of CO- andHe-WDs to investigate the formation of RCB stars. We arealso using the MESA stellar evolution and NuGridnucleosynthesis codes to construct post-merger 1Dspherical models and follow their evolution into the regionof the HR diagram where RCB stars are located.Author(s): Geoffrey Clayton (Louisiana State University), EdwardMontiel (Louisiana State University), Thomas Geballe (GeminiObservatory), Douglas Welch (McMaster University), Patrick Tisserand(Institut d'Astrophysique de Paris)

322.18 – Monitoring H-alpha Emission in BeStars of NGC 659 and NGC 663Over the past nine years we have developed a calibratedH-alpha index based on spectrophotometric data from theDominion Astrophysical Observatory 1.2-m telescope. Wehave also manufactured a set of filters to photometricallymatch our spectrophotometric band-passes. This filter set isemployed at the BYU West Mountain Observatory 0.9-mtelescope. As one of our first applications of these newfilters we examined stars in the young open clusters NGC659 and NGC 663. We were primarily interested in the Bestars and High Mass X-ray binaries in the field. From July2013 to January 2104 we observed both fields on 17 nights.We will present our preliminary results from this data set.Author(s): Eric Hintz (Brigham Young Univ.), Michael Joner (BrighamYoung Univ.)

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322.19 – Sizing Up Red Giants Using Bayes’RuleUsing the general-purpose stellar atmosphere codePHOENIX, we have constructed a grid of spherical stellaratmosphere models for comparison to cool giant starspectral energy distributions(SEDs). The models are notonly parametrized by effective temperature (3500 K to3700 K) and surface gravity (log(g) = -0.5 to 1.0), but alsoby mass (7 Msun to 21 Msun), a required parameter forspherical model atmospheres. The shapes of the syntheticspectral energy distributions are sensitive to a change inmass at fixed values for the effective temperature andsurface gravity. At our lowest surface gravity, differences inmass of a factor of two can yield up to 20% flux differencesin the shape of the SED between 400 nm and 900 nm.Also,for a fixed mass, differences in the surface gravity of afactor of 10 can yield up to 100% flux differences in theshape of the SED below 450 nm. We are investigatingwhether the mass-dependence of the model SED shapemay be used to constrain single star masses. One of ourtarget stars is the supergiant Betelgeuse which has apoorly constrained mass: published estimates differ by afactor of two. To aid in our analysis, we have developed amethod to extract Bayesian posterior distributions for fourmodel parameters (effective temperature, surface gravity,mass, and angular size) from the comparison of thesynthetic SED grid to individual observed SEDs of redgiants.Author(s): Jason Aufdenberg (Embry-Riddle Aeronautical Univ.),Tyler Parsotan (Embry-Riddle Aeronautical Univ.)

322.20 – The Complex Velocity Structure ofthe Chromosphere of VV CepheiThe eclipsing binary system VV Cephei consists of an M2Iab supergiant primary and a hotter, probably B-typemain-sequence companion. The last eclipse was observedwith the HST-STIS spectrograph at 21 epochs ranging frommid-totality through first quadrature. These observationssampled seven lines of sight through the entire, extendedchromosphere of the M supergiant star, beginning shortlyafter the hot companion emerged from total eclipse. At allseven of these egress epochs, the observed chromosphericabsorption line profiles had a typical FWHM of 25-30 km/s.These profiles contained multiple (usually two) componentsthat persisted throughout the chromosphere. The relativestrengths of the two components were observed to dependon the ionization level and excitation potential, with thelonger-wavelength (red) component tending to be strongerthan the shorter-wavelength (blue) component in thehigher-ionization and higher-excitation lines, while thestrengths of the two components were more similar inlower-excitation features. This behavior suggests the redcomponents form in hotter gas than the blue components.The great width of these chromospheric lines has beenattributed both to intrinsic chromospheric turbulence andabsorption due to the accelerating stellar wind. Here wepresent evidence that the complex absorption line profilesobserved in the extended chromosphere of VV Cep reflectan intrinsic, coherent, multi-temperature component,azimuthal velocity structure present over the entire heightof the M supergiant chromosphere, which is about a stellarradius in extent. This velocity model is inferred from thebehavior of weak ultraviolet lines of species including Al I,Ti I, Fe I, Co I, Ni I, and Zr II. We present observations,analysis of the line profile velocity structure, and discussthe implications for driving the stellar wind and associatedmass loss.Author(s): Wendy Bauer (Wellesley College), Philip Bennett (SaintMary's University)

322.21 – A New Millimeter Look at the HD15115 Debris DiskWe have used the Submillimeter Array (SMA) to make 1.3millimeter observations of the debris disk surrounding HD15115, an F-type star located in the 12 Myr-old beta Pictorismoving group. This nearly edge-on debris disk (the "BlueNeedle") has been previously well-resolved in opticalscattered light and displays an extreme asymmetry. Unlikescattered light that reflects tiny grains that are blown outby stellar radiation and swept by the interstellar medium,the thermal emission from large grains that dominate atmillimeter wavelengths closely traces the locations of thedust-producing parent planetesimals. The SMA observationsreveal a circumstellar belt of dust emission. Wecharacterize the millimeter emission using Markov ChainMonte Carlo methods to fit parametric models directly tothe visibilities and place limits on departures fromaxisymmetry.Author(s): Meredith MacGregor (Harvard-Smithsonian Center forAstrophysics), David Wilner (Harvard-Smithsonian Center forAstrophysics), Sean Andrews (Harvard-Smithsonian Center forAstrophysics), A. Hughes (Wesleyan University)

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322.22 – Resolved Multifrequency RadioObservations of GG TauWe present sub-arcsecond resolution observations ofcontinuum emission associated with the GG Tau quadruplestar system at wavelengths of 1.3, 2.8, 7.3, and 50 mm.These data confirm that the GG Tau A binary is encircled bya narrow (FWHM of 60 AU) circumbinary ring centered at aradius of 235 AU. We find no evidence for a radial gradientin the ring spectrum, suggesting that the particle sizedistribution is spatially homogeneous. A central pointsource, likely associated with the primary component (GGTau Aa), exhibits a composite spectrum from dust andfree-free emission. Faint emission at 7.3 mm is observedtoward the low-mass star GG Tau Ba, although its originremains uncertain. Using these measurements of theresolved, multifrequency emission structure of the GG Tau Asystem, models of the far-infrared to radio spectrum aredeveloped to place constraints on the grain size distributionand dust mass in the circumbinary ring. The non-negligiblecurvature present in the ring spectrum implies a maximumparticle size of 1-10 mm, although we are unable to placestrong constraints on the distribution shape. Thecorresponding dust mass is 30-300 earth masses, at atemperature of 20--30 K. We show how this significantconcentration of relatively large particles in a narrow ring at

a large radius might be produced in a local region of highergas pressures (i.e., a particle "trap") located near the inneredge of the circumbinary disk.Author(s): Sean Andrews (Harvard-Smithsonian Center forAstrophysics), Claire Chandler (National Radio Astronomy Observatory),Andrea Isella (California Institute of Technology), Tilman Birnstiel (Harvard-Smithsonian Center for Astrophysics), Katharine Rosenfeld (Harvard-Smithsonian Center for Astrophysics), David Wilner (Harvard-SmithsonianCenter for Astrophysics), Laura Perez (National Radio AstronomyObservatory), Luca Ricci (California Institute of Technology), JohnCarpenter (California Institute of Technology)

Contributing teams: Disks@EVLA

322.23 – Growth and Transport of Dust:Constraints from Circumstellar Disks andthe Solar SystemI present how dust grains in protoplanetary disks formlarger bodies and how the combined effects of dust growth,shattering, and global transport of dust aggregates shapethe observational signatures of protoplanetary disks. I willshow how observations of protoplanetary disks are able toconstrain these early stages of planet formation and howour results can be linked to properties of our own solarsystem.Author(s): Tilman Birnstiel (Harvard-Smithsonian Center forAstrophysics)

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323.01 – High Resolution Observations ofChromospheric Jets in Sunspot UmbraRecent observations of sunspot's umbra suggested that itmay be finely structured at a sub-arcsecond scalerepresenting a mix of hot and cool plasma elements. In thisstudy we report the first detailed observations of theumbral spikes, which are cool jet-like structures seen in thechromosphere of an umbra. The spikes are cone-shapedfeatures with a typical height of 0.5-1.0~Mm and a width ofabout 0.1~Mm. Their life time ranges from 2 to 3 ~min andthey tend to re-appear at the same location. Thepreliminary analysis indicates that the spikes are notassociated with photospheric umbral dots and they rathertend to occur above darkest parts of the umbra, wheremagnetic fields are strongest. The spikes exhibit up anddown oscillatory motions and their spectral evolutionsuggests that they might be driven by upward propagatingshocks generated by photospheric oscillations. It is worthnoting that triggering of the running penumbral wavesseems to occur during the interval when the spikes reachtheir maximum height.Author(s): Vasyl Yurchyshyn (Big Bear Solar Obs.), ValentynaAbramenko (Big Bear Solar Obs.), Alexander Kosovichev (Big Bear SolarObs.), Philip Goode (Big Bear Solar Obs.)

323.02 – Realistic Modeling of SpontaneousFlow Eruptions in the Quiet SunGround and space observations reveal that the solarsurface is covered by high-speed jets transporting massand energy into the solar corona and feeding the solarwind. The origin and driving forces of the observederuptions are still unknown. Using realistic numericalsimulations we find that small-scale plasma eruptions canbe produced by ubiquitous magnetized vortex tubesgenerated in the Sun's turbulent convection. The vortextubes (resembling tornadoes) penetrate into the solaratmosphere, capture and strengthen the backgroundmagnetic field, and push surrounding material up,generating impulses of Alfven waves and shocks. Oursimulations reveal complicated high-speed flows,thermodynamic, and magnetic structures in the eruptingvortex tubes. We find that the eruptions are initiated in thesubsurface layers, and initially are driven by high-pressuregradients in the subphotosphere and photosphere, and areaccelerated by the Lorentz force in the higher atmosphericlayers. The eruptions are often quasi-periodic with acharacteristic period of 2-5 min. These vortex eruptionshave a complicated flow helical pattern, with predominantlydownward flows in the vortex tube cores and upward flowsin their surroundings. For comparison with observations wecalculate full Stokes profiles in different wavelength fordifferent space and ground instruments, such as HMI/SDO,Hinode, NST/BBSO, IMaX/Sunrise. In particular, we find thatthe observed eruption events are not always associatedwith strong magnetic field concentrations, and that strongfield patches can be a source of several simultaneouseruptions.Author(s): Irina Kitiashvili (Stanford University), Seokkwan Yoon(NASA Ames Research Center)

323.03 – Theory of Collisional Two-StreamPlasma Instabilities in the SolarChromosphereThe solar chromosphere experiences intense heating justabove its temperature minimum. The heating increases theelectron temperature in this region by over 2000 K.Furthermore, it exhibits little time variation and appearswidespread across the solar disk. Although semi-empiricalmodels, UV continuum observations, and line emissionmeasurements confirm the existence of the heating, itssource remains unexplained. Potential heating sources suchas acoustic shocks, resistive dissipation, and magneticreconnection via nanoflares fail to account for the intensity,persistence, and ubiquity of the heating. Fontenla (2005)suggested turbulence from a collisional two-stream plasmainstability known as the Farley-Buneman instability (FBI)could contribute significantly to the heating. This instabilityis known to heat the plasma of the E-region ionospherewhich bears many similarities to the chromosphericplasma. However, the ionospheric theory of the FBI doesnot account for the diverse ion species found in the solarchromosphere. This work develops a new collisional,two-stream instability theory appropriate for thechromospheric plasma environment using a linear fluidanalysis to derive a new dispersion relationship and criticalE x B drift velocity required to trigger the instability. Using a1D, non-local thermodynamic equilibrium, radiative transfermodel and careful estimates of collision rates and magneticfield strengths, we calculate the trigger velocitiesnecessary to induce the instability throughout thechromosphere. Trigger velocities as low as 4 km s^-1 arefound near the temperature minimum, well below the localneutral acoustic speed in that region. From this, we expectthe instability to occur frequently, converting kinetic energycontained in neutral convective flows from the photosphereinto thermal energy via turbulence. This could contributesignificantly to chromospheric heating and explain itspersistent and ubiquitous nature.Author(s): Chad Madsen (Boston University), Yakov Dimant (BostonUniversity), Meers Oppenheim (Boston University), Juan Fontenla(NorthWest Research Associates)

323.04 – Chromospheric umbral dynamicsThe chromosphere above sunspots is seen to undergodynamical driving from perturbations from lower layers ofthe atmosphere. Umbral flashes have long been understoodto be the result of acoustic shocks due to the drop indensity in the sunspot chromosphere. Detailedobservations of the umbral waves and flashes may helpreveal the nature of the sunspot structure in the upperatmosphere. We report on high-resolution observations ofumbral dynamics observed in the Ca II 8542 line by IBIS atthe Dunn Solar Telescope. We use a principal componentdecomposition technique (POD) to isolate differentcomponents of the observed oscillations. We are able toexplore temporal and spatial evolution of the umbralflashes. We find significant variation in the nature of theflashes over the sunspot, indicating that the chromosphericmagnetic topology can strongly modify the nature of theumbral intensity and velocity oscillations.Author(s): Kevin Reardon (INAF), Antonio Vecchio (Calabria University),Gianna Cauzzi (INAF), Alexandra Tritschler (National Solar Observatory)

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323.05 – On the Signatures of Waves andOscillations in IRIS ObservationsThe objective of this study is to explore the signatures ofacoustic waves and oscillations in a variety of magneticfield configurations in the Sun’s atmosphere usinghigh-resolution spectroscopic “sit-an-stare” time seriesobtained with the Interface Region Imaging Spectrogragh(IRIS) in lines formed in the chromosphere and lowertransition region (C II 1335 & 1336, C I 1352, O I 1356, Si IV1394 & 1403 and Mg h and k). The occurrence ofoscillations in the transition region is found to stronglydepend on the magnetic field topology. The Mg h and klines reveal a particularly complex spatio-temporalbehavior. In an effort to better understand what physicalparameters can be extracted from these lines, we extendour analysis to synthetic spectra obtained from numericalsimulations and compare the results to observations.Author(s): Bernard Fleck (ESA Science Operations Department),Thomas Straus (INAF/OAC), Bart De Pontieu (LMSAL), Jorrit Leenaarts(Stockholm University), Tiago M.D. Pereira (Universtiy of Oslo)

323.06 – Investigating Molecular Hydrogenin Active Regions with IRISMolecular hydrogen should be the most abundantmolecular species in sunspots, but recent observations withIRIS show that its florescent signature is absent from abovethe sunspot umbra, but appears brightly during flares. Inthis poster we continue the analysis of FUV observations ofH2 in active regions, examining the correlation between theintensity of the H2 lines and the lines of C II and Si IV whichare responsible for their excitation. We particularly focus ondifferentiating places where H2 is abundant, holes in thechromospheric opacity where FUV photons can enter moredeeply into the solar atmosphere, and places where theFUV radiation field is intense, as in flares.Author(s): Sarah Jaeggli (Montana State University), Steven Saar(Harvard-Smithsonian Center for Astrophysics), Adrian Daw (NASAGoddard Space Flight Center), Davina Innes (Max Planck Institute for SolarSystem Research)

Contributing teams: The IRIS Team

323.07 – Asymmetric MagneticReconnection in Partially IonizedChromospheric PlasmasMagnetic reconnection is a ubiquitous process in the solarchromosphere. Realistic models of chromosphericreconnection must take into account that the plasma ispartially ionized. Asymmetric reconnection in thechromosphere may occur when newly emerged fluxinteracts with pre-existing, overlying flux. We presentsimulations of asymmetric reconnection in weakly ionized,reacting plasmas where the magnetic field strengths,densities, and temperatures are different in each upstreamregion. The simulations show considerable thinning of thecurrent sheet, asymmetric decoupling of ions and neutralsin the inflow regions, and plasmoid formation late in time.We will discuss these simulations in the context of newlyavailable observations from the Interface Region ImagingSpectrograph (IRIS).Author(s): Nicholas Murphy (Harvard-Smithsonian Center forAstrophysics), Vyacheslav Lukin (Naval Research Laboratory), JohnRaymond (Harvard-Smithsonian Center for Astrophysics)

323.09 – Jets and Bombs: CharacterizingIRIS SpectraFor almost two decades, SUMER has provided an uniqueperspective on explosive events in the lower solaratmosphere. One of the hallmark observations during thistenure is the identification of quiet sun bi-directional jets inthe lower transition region. We investigate these eventsthrough two distinct avenues of study: a MHD model forreconnection and the new datasets of the Interface RegionImaging Spectrograph (IRIS). Based on forward modelingoptically thin spectral profiles, we find the spectralsignatures of reconnection can vary dramatically based onviewing angle and altitude. We look to the IRIS data toprovide a more complete context of the chromospheric andcoronal environment during these dynamic events. Duringa joint IRIS-SUMER observing campaign, we observedspectra of multiple jets, a small C flare, and an Ellermanbomb event. We discuss the questions that arise from theinspection of these new data.Author(s): Donald Schmit (Max Planck Institute for Solar SystemResearch), Davina Innes (Max Planck Institute for Solar System Research)

323.10 – Analyzing an IRIS Blowout jet viaMagnetofrictional SimulationThe imaging spectrograph, IRIS, offers unprecedentedspatial and temporal resolution of small-scale phenomena,which allows the study of their spectral properties in thechromosphere and transition region. This study present IRISobservations of a blowout coronal jet, demonstrating theability of IRIS to detect reconnection effects in the lowatmosphere in the available suite of spectral lines. Wepresent Doppler velocity and non-thermal width (NTW)maps of the jet and their evolution in time. We interpret theresults using MHD simulations of jets. In addition, wepresent a data-driven magnetofrictional simulation of thesame jet and match the magnetic and current structure ofthe jet to the observed NTW maps. We infer the height ofthe null point and the extent of the region showingreconnection effects. We discuss the implications ofunderstanding reconnection effects in conjunction withNTW maps.Author(s): Antonia Savcheva (Harvard-Smithsonian Center forAstrophysics), Hui Tian (Harvard-Smithsonian Center for Astrophysics),Karen Meyer (Harvard-Smithsonian Center for Astrophysics)

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323.11 – Obtaining Stokes Parameters FromThe SUMI ExperimentA sounding rocket experiment designed at the MarshallSpace Flight Center, named the Solar UltravioletMagnetograph Investigation, had its second launch in Julyof 2012 to test the feasibility of measuring polarizationsignals of the ionized magnesium resonance doublet near280 nm, originating from the transition region. The rockethoused a telescope at the front end and an imaging systemat the rear end. Placed at the focal point of the self-filteringtelescope, a wave plate rotated through 12 predefinedangular orientations to restrict the measurements tospecific combinations of circular and linear polarization.Coupled with a double Wollaston analyzer, the linearlypolarized ordinary and extraordinary beams were measuredfor the 12 combinations, each containing different fractionsof the Stokes parameters (I, Q, U, V). A thorough analysis ofthe data has allowed us to come to several conclusionsregarding the design of the experiment. 1) We areconfident that polarization can be measured. A sunspotregion was determined to exhibit similar results overmultiple pixels. 2) Measurements are limited by resolution,i.e. regions smaller than the angular resolution per pixelcannot be resolved with any certainty. 3) Temporalevolution of magnetic features must be considered in futureexperimental designs. Measurements need to be taken inrepeated cycles as opposed to a single cycle over theduration of the experiment. In our presentation, we willprovide a summary of the observations along with themethods of our analysis, including the limitations thatwe’ve encountered.Author(s): Brian Fayock (University of Alabama in Huntsville), AmyWinebarger (NASA's Marshall Space Flight Center), Jonathan Cirtain(NASA's Marshall Space Flight Center), Ken Kobayashi (NASA's MarshallSpace Flight Center), Ed West (NASA's Marshall Space Flight Center)

323.12 – The Stellar-IRIS Connection: FourYears of FUV Measurements of AlphaCentauri by HST/STISSince 2010 January, shortly after the miraculous repair ofHubble's Space Telescope Imaging Spectrograph (STIS) bySM4, the two sun-like stars of Alpha Centauri ("A" [G2V]and "B" [K1V]) have been recorded on a semi-annual basisutilizing STIS's far-ultraviolet (115-170 nm) mediumresolution mode (about 8 km/s FWHM resolving power),jointly with an X-ray imaging study of AB by the ChandraObservatory. Both efforts are intended to assess thelong-term behavior of high-energy (multimillion K) coronal,and subcoronal, processes on the two relatively low-activitysolar-age dwarfs. In fact, the near-solar-twin Alpha Cen Ahas been mired in a coronal lull since 2005, originallyrecognized by XMM-Newton, and only recently has begun toclimb out of the extended X-ray minimum. Meanwhile, thelower mass, lower luminosity, but coronally more activesecondary has displayed a clear 8-year X-ray cycle,extending from the mid-1990's ROSAT era. The currentstudy focuses on properties of the "transition zone" lines(T~100,000 K) of the Alpha Centauri stars, namely the bulkredshifts exhibited by the Si IV, C IV, and N V doublets; themulti-component nature of the hot-line profiles; behavior ofthe Fe XII 124 nm coronal forbidden line; and variability ofthe FUV fluxes relative to the higher-energy X-ray timeseries. These stellar measurements, with their highprecision in wavelength and flux, complement the detailedhigh-spatial and high-temporal resolution spectral mappingof the solar corona and lower atmosphere being carried outby NASA's Interface Region Imaging Spectrograph (IRIS).[This work supported by GO grants 12758, 13060, and13465 from Space Telescope Science Institute.]Author(s): Thomas Ayres (University of Colorado)

323.13 – Brightenings Caused by FallingFilament Material on 2011 September 7Solar filaments exhibit a range of eruptive-like dynamicactivity from the full, or partial, eruption of the filamentmass and surrounding magnetic structure, as a CME, to afully confined dynamic evolution or ‘failed’ eruption. On2011 September 7, a partial eruption of a filament wasobserved by SDO and STEREO, generating a substantialstream of returning filament material that exhibited astrong interaction with the solar surface. Similarly to therecently studied 2011 June 7 event, the impact sites showclear evidence of brightening in the observed EUVwavelengths due to energy release by the impact. Weexplore two plausible physical mechanisms that wouldcause such brightening: heating of the plasma due to thekinetic energy of the impacting material - compression ofthe plasma, or reconnection between the magnetic field ofthe low-laying loops with the field carried by the impactingmaterial, or combination thereof. By analyzing the emissionof the brightenings in several SDO/AIA wavelengths, andcomparing the kinetic energy of the impacting material tothe radiative energy we provide clues for the dominantmechanism of energy release involved in the observedbrightenings. We compare this event to another in whichwe performed the same analysis (2011 June 7) where wedetermined that compression was the dominantmechanism.Author(s): Holly Gilbert (NASA's Goddard Space Flight Center),Andrew Inglis (NASA's Goddard Space Flight Center), Leila Mays (NASA'sGoddard Space Flight Center), Leon Ofman (NASA's Goddard Space FlightCenter), Elena Provornikova (NASA's Goddard Space Flight Center)

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323.14 – Characterizing and ModelingCoronal Loop BlobsThe solar corona is dominated by loop-like structures. Mostof these loops seem to be quite quiescent with a nearuniform emission along their length. However, a smallsample of loops show bright, transient blobs flowing acrosstheir length. Unlike the falling blobs observed in EIT by DeGroof et. al (2003), AIA has recorded blobs that rise fromthe base of the loop and transverse the entire loop length.A sporadic and short lived heating event is thought toinitiate the launch of a blob. However, these heating eventsare thought by some to be common in the lower solaratmosphere, so it is unclear why only a small subset ofloops should show these blobs. In this work we perform astatistical analysis on the physical properties of blobs (size,speed, intensity profile, etc.) that transverse the entire looplength. We then model a series of loops under variousheating scenarios and geometrical configurations in orderto determine which parameters play a role in blobformation.Author(s): Henry Winter (SAO), Mita Tembe (University of Virginia),Kathy Reeves (SAO), Patrick McCauley (SAO)

323.15 – A Survey of Coronal HeatingProperties in Solar Active RegionsWe investigate the properties of coronal heating in solaractive regions (AR) by systematically analyzing coronallight curves observed by the Atmospheric ImagingAssembly onboard the Solar Dynamics Observatory. Ourautomated technique computes time-lags (cooling times)on a pixel-by-pixel basis, and has the advantage that itallows us to analyze all of the coronal AR emission,including the so-called diffuse emission between coronalloops. We recently presented results using this time-laganalysis on NOAA AR 11082 (Viall & Klimchuk 2012) andfound that the majority of the pixels contained coolingplasma along their line of sight. This result is consistentwith impulsive coronal nanoflare heating of both coronalloops and the surrounding diffuse emission in the AR. Herewe present the results of our time-lag technique applied toa survey of 15 AR of different magnetic complexity, totalunsigned magnetic flux, size and age. We show that thepost-nanoflare cooling patterns identified in NOAA AR11082 are identified throughout all of the active regions inthis survey, indicating that nanoflare heating is ubiquitousin solar active regions. However, some details of thenanoflare properties, such as the nanoflare energy, aredifferent across these different active regions. We thank theSDO/AIA team for the use of these data, and the CoronalHeating ISSI team for helpful discussion of these topics.This research was supported by a NASA Heliophysics GI.Author(s): Nicholeen Viall (NASA Goddard Space Flight Center),James Klimchuk (NASA Goddard Space Flight Center)

323.16 – Imaging and Spectra of theChromosphere and Corona at the 2013 TotalEclipse in GabonWe successfully observed the 3 November 2013 eclipse's59 s of totality in clear sky from the centerline of totalitywhere it exited La Lope National Park in Gabon, close to themaximum totality available on land. Our wide-field imagingshowed two CMEs and an erupting prominence. Wecompare our images with those obtained elsewhere intotality to assess motion and dynamics. Our imagingobservations are also compared with near-simultaneousobservations from SDO/AIA, SDO/HMI, Hinode/XRT,SOHO/LASCO, SOHO/EIT, PROBA2/SWAP, andSTEREO/SECCHI. We also have flash and coronal spectra,which continue to show overall warming of the corona in2012 and 2013 through studies we have made over thesolar cycle that include the ratio of intensities of thecoronal red (Fe X 637.4 nm) and green (Fe XIV 530.3 nm)forbidden lines. The Williams College 2013 total-eclipseexpedition was supported in part by grant 9327-13 fromthe Committee for Research and Exploration of the NationalGeographic Society. Our continued work on the 2012eclipse results is supported in part by grant AGS-1047726from Solar Terrestrial Research/NSF AGS.Author(s): Jay Pasachoff (Williams College), Allen Davis (WilliamsCollege), Marek Demianski (Williams College), Vojtech Rusin (AstronomicalInstitute), Metod Saniga (Astronomical Institute), Daniel Seaton (RoyalObs.), Pavlos Gaintatzis (Aristotle U.), Aristeidis Voulgaris (Aristotle U.),Robert Lucas (U. Sydney), Zophia Edwards (Boston U.), Michael Zeiler(ESRI), Michael Kentrianakis (CBS News)

323.18 – The Coronal Global EvolutionaryModel (CGEM): Highlights of the First YearThe Coronal Global Evolutionary Model (CGEM) is a modelfor the evolution of the magnetic field in the solar corona,driven by vector and line-of-sight magnetogram data, alongwith Doppler data, taken from HMI instrument on NASA'sSDO Mission. On long time scales, the magnetic fieldevolution is computed quasi-statically using themagnetofrictional method. For a configuration whichbecomes unstable and erupts or undergoes rapid evolution,we will use the magnetofrictional configuration as the initialstate for an MHD simulation. The model will be run in bothglobal configurations, covering the entire Sun, and localconfigurations, designed to model the evolution of thecorona above active regions. In both cases, the model willuse spherical coordinates to enable a more realisticgeometry in the outer corona. The CGEM project alsoincludes the dissemination of other information derivablefrom HMI magnetogram data, such as the vertical andhorizontal Lorentz-forces computed over active regiondomains, to facilitate easier comparisons of flare/CMEbehavior and observed changes of the photosphericmagnetic field. We describe progress we have made bothon the development of this new model, and our continueddevelopment of our prototype Cartesian model, which wasthe basis for the CGEM proposal. We will discuss updatedsimulations that use our prototype model to study theevolution of NOAA AR 11158 over the time period thatincludes the 2011 February 15 X-class flare.Author(s): George Fisher (UC Berkeley)

Contributing teams: The CGEM Team (members atUCB/SSL, Stanford University, LMSAL)

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323.19 – Active Region Magnetic FieldModeling Guided by Coronal Loops andSurface FieldsDynamic events such as solar flares, filament eruptions,and mass ejections are powered by the evolving coronalmagnetic field. However, the ways in which energy isstored in, and released from, the coronal magnetic field arepoorly understood, in large part because the fieldconfiguration cannot be determined directly fromobservations and has eluded the successful application ofroutine modeling based on surface magnetograms.Recently, we have demonstrated that the Quasi-Grad-Rubin(QGR) method for modeling the current-carrying fieldassociated with active regions shows promise. InMalanushenko et al. (2014, ApJ 783:102) we have used theQGR method to construct the magnetic field at severaltimes during the evolution of AR11158 during February2011. The QGR method does not require vectormagnetograms, and instead uses the trajectories ofobserved coronal loops to constrain the locations of electriccurrents within the modeling domain. In this study, wecontinue to assess the utility of QGR by applying thismethod to additional active regions from the currentactivity cycle, making use of SDO/HMI line-of-sightmagnetograms and imagery from the extreme ultravioletchannels of SDO/AIA.Author(s): Marc DeRosa (Lockheed Martin Solar and AstrophysicsLaboratory), Anna Malanushenko (Lockheed Martin Solar andAstrophysics Laboratory), Carolus Schrijver (Lockheed Martin Solar andAstrophysics Laboratory), Michael Wheatland (University of Sydney)

323.20 – The Substructure of the SolarCorona Observed in the Hi-C TelescopeIn the summer of 2012, the High-resolution Coronal Imager(Hi-C) flew aboard a NASA sounding rocket and collectedthe highest spatial resolution images ever obtained of thesolar corona. One of the goals of the Hi-C flight was tocharacterize the substructure of the solar corona. Wetherefore calculate how the intensity scales from alow-resolution (AIA) pixels to high-resolution (Hi-C) pixelsfor both the dynamic events and “background” emission(meaning, the steady emission over the 5 minutes of dataacquisition time). We find there is no evidence ofsubstructure in the background corona; the intensity scalessmoothly from low-resolution to high-resolution Hi-C pixels.In transient events, however, the intensity observed withHi-C is, on average, 2.6 times larger than observed withAIA. This increase in intensity suggests that AIA is notresolving these events. This result suggests a finelystructured dynamic corona embedded in a smoothlyvarying background.Author(s): Amy Winebarger (NASA MSFC), Jonathan Cirtain (NASAMSFC), Leon Golub (Harvard-Smithsonian Center for Astrophysics), EdDeLuca (Harvard-Smithsonian Center for Astrophysics), Sabrina Savage(NASA MSFC), Caroline Alexander (NASA MSFC), Timothy Schuler (StateUniversity of New York College at Buffalo )

323.21 – Power Spectra in AIA 171 and 193and Their Implications for CoronalSeismologyWe examine Fourier power spectra of time-series of AIA 171and 193 waveband data. We show that these power spectraexhibit a red-noise like power-law behaviour on time-scalesof interest to coronal seismology. We show that assuming awhite noise background power spectrum when a red-noisepower spectrum is present can lead to the mistakenidentification of narrow-band oscillatory power when noneis present. This implies that a background power-law powerspectrum must be taken in to account when determiningthe presence of narrow-band oscillations that may be dueto MHD wave processes in the solar corona. We also showthat the red-noise power spectrum is consistent with theexpected power spectrum from large number ofexponentially decaying emission events with event sizetaken from a power law distribution.Author(s): Jack Ireland (ADNET Systems, NASA's GSFC), RobertMcateer (New Mexico State University), Andrew Inglis (Catholic Universityof America / NASA GSFC)

323.22 – Thermal Diagnostics with SDO/AIA:A new method and application to EruptiveActive RegionsWe present a new method for the retrieval of the emissionmeasure (EM) distribution of coronal plasma using SDO/AIAEUV images. Unlike some existing EM inversion algorithms,this inversion scheme does not make assumptions aboutthe functional form (e.g. Gaussian, power law etc.) of thesolution. The method returns positive definite solutions andruns at a speed ~O(10^4) pixels per second in a Solarsoftimplementation. We apply the method to a selection oferuptive active regions (ARs) to study the thermal evolutionof AR loops. In terms of both morphology and temporalevolution, synthetic Hinode/XRT images calculated from EMsolutions retrieved using only AIA data show goodagreement with actual XRT images.Author(s): Mark Cheung (Lockheed Martin Solar and AstrophysicsLaboratory), Paul Boerner (Lockheed Martin Solar and AstrophysicsLaboratory), Paola Testa (Smithsonian Astrophysical Observatory)

323.23 – The Sources of F10.7 EmissionThe solar radio flux at a wavelength of 10.7 cm, F10.7,serves as a proxy for the Sun’s ionizing flux striking theEarth and is a heavily used index for space weatherstudies. In principal both the coronal sources of ionizing fluxand strong coronal magnetic fields contribute to F10.7 viadifferent emission mechanisms. Recently the ExpandedVery Large Array (EVLA) has added the capability to makehigh–spatial–resolution images of the Sun at 10.7 cm. Inthis work we compare a trial F10.7 image from the EVLAwith the radio emission predicted to be present from EUVimages of the Sun acquired by the AIA telescope on theSolar Dynamics Observatory at 6 wavelengths covering thecoronal temperature range. Photospheric magnetogramsare used to identify likely regions of strong coronalmagnetic field, and the circular polarization measured bythe EVLA is used as a tracer of gyroresonance contributionsto F10.7. We discuss the conversion of the EUV data tobremsstrahlung radio fluxes via the construction ofdifferential emission measure images, and analyze therelative contributions of the different sources of F10.7 flux.Author(s): Samuel Schonfeld (New Mexico State University),Stephen White (Kirtland AFB), Carl Henney (Kirtland AFB), James McAteer(New Mexico State University), Charles Arge (Kirtland AFB)

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323.24 – Single-point Inversion of theCoronal Magnetic FieldThe Fe XIII 10747 and 10798 \AA\ lines observed in thesolar corona are sensitive to the coronal magnetic field insuch a way that, in principle, the full vector field at a pointon the line of sight can be inferred from their combinedpolarization signals. This paper presents analyticalinversion formulae for the field parameters and analyzesthe uncertainty of magnetic field measurements made fromsuch observations, assuming emission dominated by asingle region along the line-of-sight. We consider the caseof the current CoMP instrument as well as the futureCOSMO and ATST instruments. Uncertainties are estimatedwith a direct analytic inverse and with an MCMC algorithm.We find that (in effect) two components of the vector fieldcan be recovered with CoMP, and well-recovered withCOSMO or ATST, but that the third component can only berecovered when the solar magnetic field is strong andoptimally oriented.Author(s): Joseph Plowman (NCAR), Roberto Casini (NCAR), PhilipJudge (NCAR), Steven Tomczyk (NCAR)

323.25 – Observational Signatures of AlfvenWave Turbulence in Solar Coronal LoopsThe non-thermal width in coronal emission lines could bedue to the Alfven wave turbulence. In order to findobservational evidence of the Alfven waves that result incoronal heating, we examine and analyze the dynamics ofan active region observed on 2012 September 7. We usespectral line profiles of Fe XII, Fe XIII, Fe XV and Fe XVIobtained by Extreme-ultraviolet Imaging Spectrometer (EIS)on Hinode spacecraft. Line profile observations from EISwere generated and compared with our computations ofline of sight Alfven wave amplitude. We show non-thermalvelocities, Doppler outflows, and intensities for loops in thisactive region and derive comparisons between ournumerical results and observations from EIS. In ourmodeling we take into account the relationship between thewidth of the coronal emission lines and the orientation ofthe coronal loops with respect to the line-of-sight direction.We conclude that the Alfven wave turbulence model is astrong candidate for explaining how the observed loops areheated.Author(s): Mahboubeh Asgari-Targhi (Harvard-Smithsonian),Shinsuke Imada (Nagoya University), Edward DeLuca (Harvard-Smithsonian)

323.26 – First use of synoptic vectormagnetograms for global nonlinear,force-free coronal magnetic field modelsThe magnetic field permeating the solar atmosphere isgenerally thought to provide the energy for much of theactivity seen in the solar corona, such as flares, coronalmass ejections (CMEs), etc. To overcome the unavailabilityof coronal magnetic field measurements, photosphericmagnetic field vector data can be used to reconstruct thecoronal field. Currently, there are several modellingtechniques being used to calculate three dimensional fieldlines into the solar atmosphere. For the first time, synopticmaps of a photospheric vector magnetic field synthesizedfrom the vector spectromagnetograph (VSM) on SynopticOptical Long term Investigations of the Sun (SOLIS) areused to model the coronal magnetic field and estimate freemagnetic energy in the global scale. The free energy (i.e.,the energy in excess of the potential field energy) is one ofthe main indicators used in space weather forecasts topredict the eruptivity of active regions. We solve thenonlinear force free field equations using an optimizationprinciple in spherical geometry. The resulting three-dimensional magnetic fields are used to estimate themagnetic free energy content, which is the difference of themagnetic energies between the nonpotential field and thepotential field in the global solar corona. For comparison,we overlay the extrapolated magnetic field lines with theextreme ultraviolet (EUV) observations by the atmosphericimaging assembly (AIA) on board the Solar DynamicsObservatory (SDO). For a single Carrington rotation 2121,we find that the global nonlinear force free field (NLFFF)magnetic energy density is 10.3% higher than the potentialone. Most of this free energy is located in active regions.Author(s): Tilaye Tadesse Asfaw (NASA-Goddard Space FlightCenter), Alexei Pevtsov (National Solar Observatory), Peter Macneice(NASA-Goddard Space Flight Center)

323.27 – Grand Unified Speculation: CoronalCooling & Multi-thermal Analysis of AIALoopsWe have tested three controversial properties for a targetloop observed with the Atmospheric Imaging Assembly: (1)overdense loops; (2) long-lifetime loops; and (3)multithermal loops. Our loop is overdense by a factor ofabout 10 compared to results expected from steadyuniform heating models. If this were the only inconsistency,our loop could still be modeled as a single strand, but thedensity mismatch would imply that the heating must beimpulsive. Moving on to the second observable, however,we find that the loop lifetime is at least an order ofmagnitude greater than the predicted cooling time. Thisimplies that the loop cannot be composed of a single fluxtube, even if the heating were dynamic, and must be multi-stranded. Finally, differential emission measure analysisshows that the cross-field temperature of the target loop ismultithermal in the early and middle phases of its lifetime,but isothermal before it fades from view. If thesemultithermal cooling results are found to be widespread,our results could resolve the original coronal loopcontroversy of isothermal versus multithermal cross-fieldtemperatures. That is, the cross-field temperature is notalways multithermal nor is it always isothermal, butchanges as the loop cools.Author(s): Joan Schmelz (Univ. of Memphis)

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323.28 – Independent CMEs from a SingleSolar Active Region – The Case of theSuper-Eruptive NOAA AR11429In this investigation we study AR 11429, the origin of thetwin super-fast CME eruptions of 07-Mar-2012. This ARfulfills all the requirements for the 'perfect storm'; namely,Hale's law incompatibility and a delta-magneticconfiguration. In fact, during its limb-to-limb transit, AR11429 spawned several eruptions which causedgeomagnetic storms, including the biggest in Cycle 24 sofar. Magnetic Flux Ropes (MFRs) are twisted magneticstructures in the corona, best seen in ~10MK hot plasmaemission and are often considered as the culprit causingsuch super-eruptions. However, their 'dormant' existence inthe solar atmosphere (i.e. prior to eruptions), is a matter ofstrong debate. Aided by multi-wavelength and multi-spacecraft observations (SDO/HMI & AIA, HINODE/SOT/SP,STEREO B/EUVI) and by using a Non-Linear Force-Free(NLFFF) model for the coronal magnetic field, our workshows two separate, weakly-twisted magnetic flux systemswhich suggest the existence of possible pre-eruption MFRs.Author(s): Georgios Chintzoglou (Naval Research Laboratory),Spiros Patsourakos (University of Ioannina), Angelos Vourlidas (NavalResearch Laboratory)

323.29 – Findings from a Three Year Surveyof Coronal Null PointsWe report the findings from a comprehensive coronalmagnetic null point survey created by Potential Field SourceSurface (PFSS) modeling & Solar DynamicObservatory/Atmospheric Imaging Assembly (SDO/AIA)observations. Locations of magnetic null points in thecorona were predicted from the PFSS model fromCarrington Rotation 2098 to 2139 and manually comparedto contrast enhanced SDO/AIA images in 171 angstroms.Statistical results will be presented that illustrate thecharacteristics associated with the observed and predictednull points. These characteristics include the radial &latitudinal distribution; eigenvalues associated with nullpoint structure; and the effect spine orientation has onobservability.Author(s): Michael Freed (Montana State University), DanaLongcope (Montana State University), David McKenzie (Montana StateUniversity)

323.30 – Validation of SphericallySymmetric Inversion by Use of aTomographic Reconstructed Three-Dimensional Electron Density of the SolarCoronaDetermination of the coronal electron density by theinversion of white-light polarized brightness (pB)measurements by coronagraphs is a classic problem insolar physics. An inversion technique based on thespherically symmetric geometry (Spherically SymmetricInversion, SSI) was developed in the 1950s, and has beenwidely applied to interpret various observations. In thisstudy we present the detailed assessment of this methodusing a model in terms of three-dimensional (3D) electrondensity in the corona from 1.5 to 4 solar radii reconstructedby tomography method from STEREO/COR1 observations.We first show in theory and observation that the sphericallysymmetric polynomial approximation (SSPA) method andthe Van de Hulst inversion technique are equivalent. Thenwe assess the SSPA method using synthesized pB imagesfrom the 3D density model, and find that the SSPA densityvalues for edge-on streamers are very close to the modelinputs in the plane of sky with differences generally lessthan a factor of two or so; the SSPA density has the lowerpeak but more spread in latitudinal direction than in themodel. Our results confirm the previous suggestion that theSSI method is very suitable to streamers in the solarminimum. In addition, we demonstrate that the SSPAmethod can be used to reconstruct the 3D coronal density,roughly in agreement with that by tomography in a periodof low solar activity. We suggest that the SSI method iscomplementary to the 3D tomographic technique in somecases, given that the development of the latter is still anongoing research effort.Author(s): Tongjiang Wang (Catholic Univ of America / NASAGSFC), Maxim Kramar (Catholic Univ of America / NASA GSFC), JosephDavila (NASA Goddard Space Flight Center)

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323.31 – A Comparison Study of TwoNeighboring Eruptive and Non-EruptiveFilamentsWe perform a comparison study of an eruptive filament inAR 11283 and a nearby quiescent filament. The coronalmagnetic field supporting these two filaments isextrapolated using a CESE-MHD-NLFFF code (Jiang et al.2013, Jiang et al. 2014), which presents two magnetic fluxropes (FRs) in the same extrapolation box. The numericallyreproduced magnetic dips of the FRs match observations ofthe filaments strikingly well, which supports strongly theFR-dip model for filaments. The FR that supports the AReruptive filament is much smaller (with length of 30~Mm)compared with the large-scale FR holding the quiescentfilament (with length of 300~Mm). But the AR eruptive FRcontains most of the magnetic free energy in theextrapolation box and holds a much higher magneticenergy density than the quiescent FR, because it residesalong the main polarity inversion line (PIL) around sunspotswith strong magnetic shear. Both the FRs are weaklytwisted and cannot trigger kink instability. The AR eruptiveFR is unstable because its axis reaches above a criticalheight for torus instability (TI), at which the overlyingclosed arcades can no longer confine the FR stably. On thecontrary, the quiescent FR is very firmly held by itsoverlying field, as its axis apex is far below the TI thresholdheight. (This work is supported by NSF)Author(s): Chaowei Jiang (The University of Alabama inHuntsville), S. Wu (The University of Alabama in Huntsville), XueshangFeng (Center for Space Science and Applied Research, Chinese Academyof Sciences), Qiang Hu (The University of Alabama in Huntsville)

323.32 – Solar Coronal Temperature Duringthe Rise of Cycle 24Observations of the solar corona are obtained with thephotoelectric coronal photometer fed by the 40-cmcoronagraph in the John W. Evans Solar Facility at theNational Solar Observatory at Sacramento Peak in Sunspot,NM. The observations consist of daily scans every 3° inlatitude at 1.15 solar radii in Fe XIV 530.3 nm and Fe X637.4 nm. The scans were obtained from 1983 to 2013. Thecoronal temperature (Tc) may be calculated as a function ofthe ratio of the intensities of Fe XIV and Fe X, as shown byGuhathakurta, Fisher and Altrock (1993, Astrophys. J. Lett.,414, L145). In this paper, I use this technique to study thelong-term, large-scale variation of Tc over the last 3 solarcycles. The observations are used to determine thevariation of Tc at latitudes above 30°. Latitudes below 30°are not studied, because the technique used to determineTc is not applicable to active regions, where the assumptionof a uniform temperature along the line-of-sight is deniedby the presence of many active-region loops of varyingtemperatures. Suitable temporal averages are taken toreduce noise. Prior to the last solar minimum we find that(i) a well-defined solar-cycle variation of Tc at 1.15 Ro wasseen, varying by 0.4 MK near the poles, (ii) Tc near solarminimum decreased strongly toward the poles above 60°latitude, and (iii) a variation ~ 0.1 MK was seen in theaverage Tc above 30° latitude. However, since the last solarmaximum, we show that the pattern established during theprevious two cycles was broken. The most important newconclusions are Tc since minimum reached maximumearlier in the North than in the South, and Tc at themaximum of Cycle 24 is significantly lower than inprevious cycles. We also found that (i) the polar Tc onlydecreased by 0.3 MK from solar maximum to minimuminstead of 0.4 MK, (ii) Tc near solar minimum did notdecrease strongly toward the poles above 60° latitude,which it did in earlier cycles, (iii) the average Tc above 30°latitude reached a record low value of 1.4 MK, but theminimum polar Tc was 0.13 MK hotter than the previouscycle, and (iv) the latitude-variation of Tc at solar minimumwas less than 0.1 MK.Author(s): Richard Altrock (Air Force Research Laboratory)

323.33 – Photospheric Signatures of CoronalHole JetsCoronal jets are transient, collimated ejections of plasmathat are a common feature of solar X-ray and EUV imagesequences. Of special interest is the contribution thatcoronal hole jets make to the solar wind outflow. A newclass of coronal hole jets, termed "dark jets", has beenidentified with the EUV Imaging Spectrometer (EIS) onboard Hinode. The jets are identified in EUV spectral lineswith line-of-sight velocities of 50-100 km/s and enhancedline widths, yet they show little or no intensity signature inimage sequences from the Atmospheric Imaging Assemblyon board the Solar Dynamics Observatory (SDO) or theX-Ray Telescope on board Hinode. In this contribution wewill investigate the photosphere at the footpoint of thesejets. White light images from the Helioseismic MagneticImager (HMI) on board SDO are used to derive the plane-of-sky flow field using local correlation tracking, and HMImagnetograms show the evolution of the magnetic flux.Both the evolution of the magnetic field and flows allow usto study the photospheric driver of these jets.Author(s): Karin Muglach (Artep, Inc), Peter Young (GMU)

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323.34 – Simulations on Coronal Jets withThermal ConductionObservations by Yohkoh, SOHO, Hinode and STEREO showthat X-ray jets in the coronal holes, with an inverse-Y shape,occur at a rate of about 60 jets/day, and have a typicaloutward velocity of 160km/s, height of 50 Mm and width of8 Mm, and liftime of 10 min (Savcheva et al., 2007).Numerical simulations suggest that jets are related to thereconnection between the newly emerging and pre-existingmagnetic fields. We here study the eruption of coronal jetsby MHD simulations of flux emergence into the corona withambient fields. Reconnection of the emerging and ambientfields converts magnetic energy into thermal and kineticenergy of the plasma, capturing the statistical properties ofcoronal jets. Interesting features of observed jets, such asthe twisting motion sigmoidal current structure are alsoproduced in our simulations. In addition, we implementedheat conduction along the field lines to produce a morerealistic structure along the field lines, which allows us tocompare the synthetic images with AIA observations.Author(s): Fang Fang (High Altitude Observatory), Yuhong Fan (HighAltitude Observatory)

323.36 – MHD Modeling of Coronal HoleEvolutionMHD simulations of the solar corona based on maps of thesolar magnetic field have been demonstrated to describemany aspects of coronal structure. However, these modelsare typically integrated to steady state, using synoptic ordaily-updated magnetic maps to derive the boundaryconditions. The Sun's magnetic flux is always evolving, andthese changes in the flux affect the structure and dynamicsof the corona and heliosphere. In this presentation, wedescribe an approach to evolutionary models of the coronaand solar wind, using time-dependent boundary conditions.A key aspect of our approach is the use of the Air ForceData Assimilative Photospheric flux Transport (ADAPT)model to develop time-evolving boundary conditions for themagnetic field. In this study, we use a simplified (zero-beta)MHD model to investigate coronal hole evolution during theJune-August 2010 time period (Carrington rotations2098-2099). We compare modeled and observed coronalholes, and discuss implications of coronal hole evolution forthe origin of the slow solar wind.Author(s): Jon Linker (Predictive Science Inc), Roberto Lionello(Predictive Science Inc), Cooper Downs (Predictive Science Inc), RonCaplan (Predictive Science Inc), Zoran Mikic (Predictive Science Inc), PeteRiley (Predictive Science Inc), Carl Henney (Air Force Research Laboratory),Charles Arge (Air Force Research Laboratory)

323.37 – Statistical Properties of Jets in theSDO EraWe examine the statistical properties of jets observed inX-ray and EUV since the launch of the Solar DynamicsObservatory (SDO). We identify over 150 jets using datafrom Hinode X-ray Telescope (XRT) coronal hole observingcampaigns and examine their properties using SDOAtmospheric Imaging Array (AIA) . Each event is identifiedas type 1 (classic jet), type 2 (blowout jet ) or type 3(indeterminable). We calculate their intensity, lifetime,apparent velocity, angle of inclination and note if they areassociated with a bright points. This study will be used forthe validation of the Automatic Jet Detection Module; partof the SDO Feature Finding Team.Author(s): Samaiyah Farid (University of Alabama Huntsville),Antonia Savcheva (Smithsonian Astrophysical Observatory )

323.38 – A Comparison of EUV Coronal HoleMeasurements and Modeled Open MagneticFieldCoronal holes are regions on the Sun's surface that map thefootprints of open magnetic field lines. We have developedan automated routine to detect and track boundaries oflong-lived coronal holes using full-disk extreme-ultraviolet(EUV) images obtained by SOHO/EIT, SDO/AIA, andSTEREO/EUVI. Using these observations in conjunction withthe potential field source surface (PFSS) model, we find thatfrom 1996 through 2010, coronal holes extend between 5%and 17% of the solar surface area, with total unsigned open

flux varying between (2-5)x1022 Mx. AIA/EUVImeasurements spanning 2010 through 2013 mark coronalhole coverage areas of 5% to 10% of total solar surfacearea, with total unsigned open magnetic flux ranging from

(2-4)x1022 Mx. A detailed comparison indicates thatcoronal holes in low latitudes significantly contribute to thetotal open magnetic flux. Previous studies using the He I10830 line or EIT EUV images do not always accuratelymeasure these low latitude coronal holes. Enhancedobservations from AIA/EUVI in conjunction with anobservation-driven flux transport model allow a moreaccurate measure of these low latitude coronal holes andtheir resulting contribution to solar open magnetic flux.Author(s): Chris Lowder (Montana State University), Jiong Qiu(Montana State University), Robert Leamon (Montana State University),Dana Longcope (Montana State University), Yang Liu (Stanford University)

323.39 – Further Analysis of Active RegionThermal Structure from EUNIS-13The 2013 April 23 flight of the Extreme Ultraviolet NormalIncidence Spectrograph (EUNIS) sounding rocket instrumentreturned high-quality spectra in two wavelength bands,30.0-37.0 nm and 52.7-63.5 nm, sampling three activeregions (11723, 11724, and 11726). The spectral lines inthese bands probe a wide temperature range, 0.03 MK to 8MK. We have demonstrated that the differential emissionmeasure (DEM) varies significantly between differentsub-regions of AR 11726. We extend this analysis to ARs11723 and 11724 and include a wider selection of spectrallines to delineate better the variations in thermal structure.Author(s): Douglas Rabin (NASA Goddard Space Flight Center),Enrico Landi (University of Michigan), Adrian Daw (NASA Goddard SpaceFlight Center), Jeffrey Brosius (NASA Goddard Space Flight Center)

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323.40 – Computing EUV and Soft X-raysEmissions from an Active Region in 3DEUV and soft X-rays can be a useful tool for plasmadiagnostics when applied to an active region. Instead oftrying to unfold the plasma properties from the observedemissions, we use a forward modeling method on AR 7986.Namely, we first compute the thermal structure of theactive region. The resulting density and temperatureprofiles are then used to compute the expected emissions,and the synthetic images are compared with observations.Our model reproduces many features of an observed activeregion, including a dark neutral line, coronal loops, fanloops, etc. The time evolution of the emissions showplasma flows that resemble coronal rains. Quantitatively,the coronal part of the loops compare favorably withobservations on all three coronal lines of EIT, although theirfootpoints are somewhat brighter than observed. Thediscrepancy may be attributed to the inaccurateabundances used to compared the emissions in the lowcorona and below. Work supported by the HeliophysicsTheory Program of NASA.Author(s): Yung Mok (Univ. of California, Irvine), Roberto Lionello(Predictive Science, Inc.), Zoran Mikic (Predictive Science, Inc.), Jon Linker(Predictive Science, Inc.)

323.41 – Thermal Non-equilibriumConsistent with Widespread CoolingTime correlation analysis has been used to showwidespread cooling in the solar corona; this cooling hasbeen interpreted as a result of impulsive (nanoflare)heating. In this work, we investigate wide-spread coolingusing a 3D model for a solar active region which has beenheated with highly stratified heating. This type of heatingdrives thermal non-equilibrium solutions, meaning thatthough the heating is effectively steady, the density andtemperature in the solution are not. We simulate theexpected observations in narrowband EUV images andapply the time correlation analysis. We find that the resultsof this analysis are qualitatively similar to the observeddata. We discuss additional diagnostics that may be appliedto differentiate between these two heating scenarios.Author(s): Amy Winebarger (NASA MSFC), Roberto Lionello (PredictiveScience, Inc), Zoran Mikic (Predictive Science, Inc), Jon Linker (PredictiveScience, Inc), Yung Mok (University of California)

323.42 – The Onset of MagneticReconnection in the Solar AtmosphereA fundamental question concerning magnetic energyrelease on the Sun is why the release occurs only aftersubstantial stresses have been built up in the field. Ifreconnection were to occur readily, then the releasedenergy would be much less than the energy required forcoronal heating, CMEs, flares, jets, spicules, etc. How canwe explain this switch-on property? What is the physicalnature of the onset conditions? One idea involves the"secondary instability" of current sheets, which switches onwhen the rotation of the magnetic field across a currentsheet reaches a critical angle. Such conditions would occurat the boundaries of flux tubes that become tangled andtwisted by turbulent photopheric convection, for example.Other ideas focus on a critical thickness for the currentsheet. We report here on the preliminary results of ourinvestigation of reconnection onset. Unlike our earlier workon the secondary instability (Dahlburg, Klimchuk, andAntiochos 2005), here we treat the coupled chromosphere-corona system. Using the BATS-R-US MHD code (Toth et al.2012), we simulate a single current sheet in a shearedmagnetic field that extends from the chromosphere into thecorona. Driver motions are applied at the base of themodel. The configuration and chromosphere are bothidealized, but capture the essential physics of the problem.The advantage of this unique approach is that it resolvesthe current sheet to the greatest extent possible whilemaintaining a realistic solar atmosphere. It thus bridges thegap between "reconnection in a box" studies and studies oflarge-scale systems such as active regions. One questionwe will address is whether onset conditions are met first inthe chromosphere or corona.Author(s): Rebekah Evans (NASA Goddard Space Flight Center),James Klimchuk (NASA Goddard Space Flight Center), Bart Van Der Holst(University of Michigan)

323.43 – Coronal Seismology: InferringMagnetic Fields and Exploring DampingMechanismsCoronal seismology provides a method to both infer coronalplasma parameters and to differentiate between potentialdamping mechanisms. We study a complex set of flare-induced, off-limb, coronal kink-mode oscillations. There areover 100 loops that display a spread of periods, amplitudes,and damping times. These are used to create a coronalmagnetic field map, where the behavior of each loop allowsfor the magnetic field strength to be determined on acase-by-case basis. We show that both Fourier and Waveletroutines can be used to automatically extract andcharacterize such oscillations, and therefore can providesuch magnetic field maps in a near-realtime setting. Westudy the damping lengths and times to differentiatebetween several damping mechanisms. Resonantabsorption and phase mixing are both in agreement withthe damping parameters in this event, with resonantabsorption appearing the simplest explanation. We explorehow such studies can now be carried out across allavailable SDO EUV passbands.Author(s): James McAteer (New Mexico State University), JackIreland (NASA GSFC), Andrew Inglis (NASA GSFC)

Contributing teams: SDO Feature Finding Team

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323.44 – Advection of Magnetic Field Linesin Supra-Arcade Fan StructuresRecent attempts to characterize the apparent motion ofsupra-arcade fan structures have revealed bulk velocityand displacement spectra that may give insights into theenergy distribution in supra-arcade plasma sheets. In orderto form a more complete picture of the energy balance inthese structures it is important to understand the magneticfield on a similar scale. In this work we used velocity mapsfound through local correlation tracking (LCT) as sourcefunctions for a 2D, time-dependent, ideal inductionequation. We began with an assumed initial configurationand then evolved the magnetic field in order to maintainthe frozen-in condition. We then characterized the energydeposition into the field as well as the field strengthspectrum and several other quantities of interest. It is ourhope that this study will serve to improve ourunderstanding of the interplay between the plasma and themagnetic field in the supra-arcade region.Author(s): Roger Scott (Montana State University), Michael Freed(Montana State University), David McKenzie (Montana State University),Dana Longcope (Montana State University)

323.45 – Coronal Magnetography of aSimulated Solar Active Region fromMicrowave Imaging SpectropolarimetryWe have simulated the Expanded Owens Valley Solar Array(EOVSA) radio images generated at multiple frequenciesfrom a model solar active region, embedded in a realisticsolar disk model, and evaluated the resulting datacube fordifferent spectral analysis schemes to evaluate thepotential for realizing one of EOVSA's most importantscientific goals — coronal magnetography. In this paper, wefocus on modeling the gyroresonance and free-freeemission from an on-disk solar active region model withrealistic complexities in electron density, temperature andmagnetic field distribution. We compare the magnetic fieldparameters extrapolated from the image datacube alongeach line of sight after folding through the EOVSAinstrumental profile with the original (unfolded) parametersused in the model. We find that even the most easilyautomated, image-based analysis approach (Level 0)provides reasonable quantitative results, although they areaffected by systematic effects due to finite sampling in theFourier (uv) plane.Author(s): Zhitao Wang (New Jersey Institute of Technology), DaleGary (New Jersey Institute of Technology), Stephen White (Air ForceResearch Laboratory)

323.46 – Magnetic reconnection and tearingin a 3D current sheet about a solar coronalnullThree-dimensional magnetic null points are ubiquitous inthe solar corona and in any generic mixed-polaritymagnetic field. We discuss the nature of flux transfer duringreconnection an isolated coronal null point, that occursacross the fan plane when a current sheet forms about thenull. We then go on to discuss the breakup of the currentsheet via a non-linear tearing-type instability and show thatthe instability threshold corresponds to a Lundquist numbercomparable to the 2D case. We also discuss the resultingtopology of the magnetic field, which involves a layer inwhich open and closed magnetic fields are effectivelymixed, with implications for particle transport.Author(s): David Pontin (University of Dundee), Peter Wyper(University of Dundee)

323.47 – Visibility of Extended CoronalStructures and CMEs in the EUVExtended coronal structures around active regions andcoronal mass ejections (CMEs) have often been seen in theextreme-ultraviolet (EUV) channels to the full extent of theAIA and SWAP field of views (~1.3 and 1.7 Rsun). Usingoff-pointed comet data in AIA we sum a large number offrames to evaluate the off-limb distance to which streamerscan be detected. For CMEs, we compared the eventsclassified as halo CMEs in the white-light LASCO CACTuscatalog from July-September 2013 to the AIA and SWAPdata collected around those events. We discovered thatroughly 80% of events could be seen in the EUV using bothregular and running difference movies, with the mosteffective channels being the 193 and 304Å channels. Byprojecting out the signal strength of several of theseevents, we conclude that these EUV events can in manycases be detected to over 2.5 Rsun. A larger field-of-viewtelescope would make it possible to track the developmentof these structures and events from the disk out to severalsolar radii, complementing the traditional white-lightmethods.Author(s): Nicole Schanche (SAO), Leon Golub (SAO)

323.48 – Waves and jets in coronal loops:the effects of radiative coolingObservations with Hinode/EIS of coronal loops in solaractive regions revealed that propagating disturbances ofEUV intensity are associated with plasma upflows or jets atloops footpoints. To investigate the excitation and evolutionof waves due to plasma jets, we expand recent studies withmore realistic 3D MHD model that includes full energyequation with empirical heating and radiative coolingterms. We perform 3D MHD simulations of loops byapplying different flow drivers at the loops footpoints, asingle upflow pulse and a broadband excitation of smallamplitude (subsonic) velocity pulses. Parameters of thepulses are chosen according to the observed properties. Weinitialize the computations with an equilibrium state of amodel active region using potential (dipole) magnetic field,gravitationally stratified density and temperature obtainedfrom polytropic equation of state of the background coronalplasma. We study the initiation and the dynamics of plasmaflows, excitation and damping of waves, and flow-waveinteractions in the loops for various forms of heating. Weinvestigate the effects of radiation losses on the dampingof MHD waves on the jets in coronal loops.Author(s): Elena Provornikova (NASA Goddard Space FlightCenter), Leon Ofman (NASA Goddard Space Flight Center), TongjiangWang (NASA Goddard Space Flight Center)

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323.49 – MESSENGER soft X-rayobservations of the quiet solar coronaIn a remarkable result from their "SphinX" experiment,Sylwester et al. (2012) found a non-varying base level ofsoft X-ray emission at the quietest times in 2009. Wedescribe comparable data from the soft X-ray monitor onboard MESSENGER (en route to Mercury) which hadexcellent coverage both in 2009 and during the true solarminimum of 2008. These observations overlap SphinX's andalso are often exactly at Sun-MESSENGER-Earthconjunctions. During solar minimum the Sun-MESSENGERdistance varied substantially, allowing us to use theinverse-square law to help distinguish the aperture flux (ie,solar X-rays) from that due to sources of background in the2-5 keV range. The MESSENGER data show a non-varyingbackground level for many months in 2008 when no activeregions were present. We compare these data in detail withthose from SphinX. Both sets of data reveal a differentbehavior when magnetic active regions are present on theSun, and when they are not. Reference: Sylwester et al., ApJ751, 111 (2012)Author(s): Richard Schwartz (NASA's GSFC), Hugh Hudson (Universityof Glasgow), Anne Tolbert (NASA's GSFC), Brian Dennis (NASA's GSFC)

323.50 – A study on the sensitivity ofoutflow velocity determinations for coronalstreamers made within 2.5 solar radiiOutflow velocity determinations in coronal streamers havebeen traditionally studied using the Doppler dimmingtechniques (SOHO/UVCS) and correlation tracking ofbrightness irreqularities (blobs) with white lightcoronagraphs. These velocity measurements are in theplane of sky, approximately transverse to the line of sight.The earlier UVCS outflow measurements are not verysensitive for low outflows (V < 30 km/s) and the white lightcoronagraphs probably have similar uncertainties. We havestarted a new streamer study which uses the approach ofNoci & Gavryuseva (2007) to determine outflow velocitiesas low as 20 km/s in the plane of the sky. This study isbeing used to improve the mapping of solar wind outflow inthe transition between open and mainly closed magneticfield regions on the boundaries of coronal streamers. Weshow initial results using data from SOHO observations anddiscuss their relevance to mechanisms for generating theslow solar wind.Author(s): Leonard Strachan (Harvard-Smithsonian, CfA)

323.51 – Solar Polar Jets Driven by MagneticReconnection, Gravity, and WindPolar jets are dynamic, narrow, radially extended structuresobserved in solar EUV emission near the limb. Theyoriginate within the open field of coronal holes in“anemone” regions, which are intrusions of oppositemagnetic polarity. The key topological feature is a magneticnull point atop a dome-shaped fan surface of field lines.Applied stresses readily distort the null into a current patch,eventually inducing interchange reconnection between theclosed and open fields inside and outside the fan surface(Antiochos 1996). Previously, we demonstrated thatmagnetic free energy stored on twisted closed field linesinside the fan surface is released explosively by the onsetof fast reconnection across the current patch (Pariat et al.2009, 2010). A dense jet comprised of a nonlinear, torsionalAlfvén wave is ejected into the outer corona along thenewly reconnected open field lines. Now we are extendingthose exploratory simulations by including the effects ofsolar gravity, solar wind, and expanding sphericalgeometry. We find that the model remains robust in theresulting more complex setting, with explosive energyrelease and dense jet formation occurring in the low coronadue to the onset of a kink-like instability, as found in theearlier Cartesian, gravity-free, static-atmosphere cases. Thespherical-geometry jet including gravity and windpropagates far more rapidly into the outer corona and innerheliosphere than a comparison jet simulation that excludesthose effects. We report detailed analyses of our newresults, compare them with previous work, and discuss theimplications for understanding remote and in-situobservations of solar polar jets. This work was supported byNASA’s LWS TR&T program.Author(s): C. DeVore (NASA GSFC), Judith Karpen (NASA GSFC), SpiroAntiochos (NASA GSFC)

323.52 – A Solar Coronal Cavity with a HotCore Observed by HinodeCoronal cavities are large low density regions oftenobserved above high latitude filament channels. Thesecavities will sometimes have areas of bright X-ray emissionnear their centers. Using Hinode satellite data from theX-ray Telescope (XRT) and the EUV Imaging Spectrometer(EIS) we examine the thermal emission properties andcoronal velocity structures of a cavity, containing a centralbright X-ray emission, observed on 23 February 2012. Weinvestigate the interaction between the coronal cavity andthe prominence material using data from the AtmosphericImaging Assembly (AIA) aboard the Solar DynamicObservatory (SDO) and H-? data from the Hinode SolarOptical Telescope (SOT). We use a non-linear force-free fieldmodel to understand the magnetic field structure that givesrise to the coronal emission in this cavity. A comparison ofAIA and XRT data reveal emission in 171 that outlines thehot core of the cavity; consistent with the modeledmagnetic field structure. This work is supported by undercontract SP02H1701R from Lockheed-Martin to SAO,contract NNM07AB07C from NASA to SAO and grantnumber NNX12AI30G from NASA to SAO.Author(s): Patricia Jibben (Harvard-Smithsonian Center forAstrophysics), Kathy Reeves (Harvard-Smithsonian Center forAstrophysics), Yingna Su (Harvard-Smithsonian Center for Astrophysics)

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323.53 – Hinode/EIS observationssignatures of plume and interplumeregions.Alfven waves are a very promising mechanism to explainthe process by which energy is transported from the solarsurface into the solar corona and then dissipated by variousprocess, thereby heating the solar corona and driving thesolar wind. Recent work has shown that Alfven waves bothcarry and dissipate enough energy to heat coronal holesand accelerate the fast solar wind. Within coronal holes,one finds plumes, relatively bright, narrow structures,coinciding with open magnetic field lines. They expandfrom the chromosphere far out into the solar corona. Manyaspects of these structures remain poorly understood, suchas their morphology and their contribution to the fast solarwind. More specifically, it is not known whether the plumeor interplume regions are the preferred channel forsupplying material into the fast solar wind. In this work, weinvestigate spectroscopically the properties of both plumeand interplume regions, using Hinode/EIS observationsduring the recent solar minimum. In particular, we focus ondetermining the wave properties of the gas, through theanalysis of EUV line width variations. The presence of suchwaves broadens spectral lines in proportion to the waveamplitude. By separating both the thermal and non-thermalbroadening, we can determine the energy carried by waveswithin such structures as well as the ion temperatures.Density and additional temperatures diagnostics are alsoused allowing us to further characterize the coronal plasma.Author(s): Chloe Guennou (Columbia astrophysics Laboratory),Daniel Savin (Columbia astrophysics Laboratory), Michael Hahn (Columbiaastrophysics Laboratory)

323.54 – SDO/AIA observations and modelof standing waves in hot coronal loopsexcited by a flareThe strongly damped Doppler shift oscillations in hotcoronal loops were first observed by SOHO/SUMER in flarelines formed at plasma temperature more than 6 MK. Theywere mainly interpreted as the standing slow magnetosonicwaves excited by impulsive energy release at the loop’sfootpoint based on the measured properties and on MHDmodeling results. Longitudinal waves with similar propertieshave been recently observed by SDO/AIA in active regionloops. In this study, we report a new event that exhibitedthe flare-excited intensity disturbances propagating backand forth in a hot coronal loop imaged by AIA in 131bandpass. We measure the physical parameters of thewave and loop plasma, determine the loop geometry, andexplore the triggering mechanism. We identify the wavemodes (propagating or standing waves) based on thesemeasurements and on 3D MHD modeling. A loop model isconstructed with enhanced density in a hydrostaticequilibrium following potential or force-free magnetic fieldlines extrapolated from the photospheric magnetic fielddata observed by SDO/HMI. We also discuss theapplications of coronal seismology to this event.Author(s): Tongjiang Wang (Catholic Univ of America / NASAGSFC), Leon Ofman (Catholic Univ of America / NASA GSFC), ElenaProvornikova (Catholic Univ of America / NASA GSFC), Joseph Davila(NASA's GSFC)

323.55 – Coronal Cavity Catalog from SDOObservationsWe present a catalog of coronal cavities and prominencesassociated with cavities since the launch of Solar DynamicsObservatory (SDO). Coronal cavities are dark, circularregions observed above the solar limb in white light andEUV coronal images. They are believed to be regions oflower density relative to the surrounding corona. We usesynoptic maps made from EUV images from theAtmospheric Imager Assembly (AIA) instrument on boardSDO to study coronal cavities. The synoptic maps,constructed from annuli above the solar limb, best showcavities in 211 A (Fe XIV, 2.0 MK) and 193 A (Fe XII, 1.6 MK)and 171 A (Fe IX, 0.6 MK) passbands. Moreover, 304 A (HeII, 0.05 MK) synoptic maps best show the evolution of anyprominences associated with a cavity. The catalog lists thenumber of cavities seen in each Carrington rotation startingfrom CR 2097, the cavity’s size, shape, and theheliographic longitudes and latitudes of the appearanceand disappearance of the cavity. Our goal is to provide aconsistent set of the cavity structures for broad scientificuse.Author(s): Nishu Karna (NASA GSFC), Jie Zhang (George MasonUniversity), William Pesnell (NASA GSFC), Shea Hess Webber (NASA GSFC)

323.56 – Untangling Coronal Streamersfrom PseudostreamersWe study the coronal source regions of the solar wind -- inparticular the coronal streamers and pseudostreamers thatare believed to be the sources of slow wind streams -- withmulti-spacecraft and ground-based observations. Due tothe large number of both unipolar pseudostreamers andclassical bipolar helmet streamers and their longpersistence over multiple solar rotations, their relativecontributions to the solar wind are likely to be substantial.We compare the physical properties of selected helmetstreamers and pseudostreamers to characterize how thedifferences in magnetic topology affect the plasmaproperties of the coronal structures. In order to investigateslow solar wind heating and acceleration, we also compareour measurements with predictions from streamer andpseudostreamer theoretical models. This work is supportedby NASA grant NNX10AQ58G to the SmithsonianAstrophysical Observatory.Author(s): Mari Paz Miralles (Harvard-Smithsonian CfA), StevenCranmer (Harvard-Smithsonian CfA), Guillermo Stenborg (George MasonUniversity)

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323.58 – Solar Energetic Particle Events inDifferent Types of Solar WindWe examine statistically some properties of 96 20 MeVgradual solar energetic proton (SEP) events as a function ofthree different types of solar winds (SWs) as classified byRichardson and Cane (2012). Gradual SEP (E > 10 MeV)events are produced in shocks driven by fast (V > 900km/s) and wide (W > 60 deg) coronal mass ejections(CMEs). We find no differences between transient and fastor slow SW streams for SEP 20-MeV event timescales. It hasrecently been found that the peak intensities Ip of theseSEP events scale with the ~ 2 MeV proton backgroundintensities, which may be a proxy for the near-Sun shockseed particles. Both the intensities Ip and their 2 MeVbackgrounds are significantly enhanced in transient SWcompared to those of fast and slow SW streams, and thevalues of Ip normalized to the 2 MeV backgrounds onlyweakly correlate with CME V for all SW types. This resultimplies that forecasts of SEP events could be improved bymonitoring both the Sun and the local SW streamproperties and that the well known power-law sizedistributions of Ip may differ between transient andlong-lived SW streams. We interpret an observedcorrelation between CME V and the 2 MeV background forSEP events in transient SW as a manifestation of enhancedsolar activity.Author(s): Stephen Kahler (Air Force Research Laboratory), AngelosVourlidas (Naval Research Laboratory)

323.59 – Taking Extreme Space Weather tothe Milky WayExtreme Space Weather events are large solar flares orgeomagnetic storms, which can cause economic damagethat cost billions of dollars to recover from. We have fewexamples of such events; only the Carrington Event (thesolar superstorm) has superlatives in three categories: sizeof solar flare, drop in Dst, and amplitude of aa. Keplerobservations show that stars similar to the Sun can haveflares releasing thousands of times more energy than anX-class flare. These flares would strongly affect theatmosphere surrounding a planet orbiting such a star.Particle and magnetic field outflows from these stars couldalso be present. We are investigating the level of solaractivity that is necessary to strongly affect the atmosphereof terrestrial planets. We assume that a habitable planetrequires an atmosphere with a temperature andcomposition that is stable in time. Can we then extrapolateresults from our solar system to determine a space ofstellar parameters in which habitable planets can exist?Author(s): W. Pesnell (NASA GSFC)

323.60 – Validating solar wind predictionusing the Current Sheet Source SurfacemodelWe have carried out a comparative study of the predictedsolar wind based on the flux tube expansion factor (FTE)computed using the Current Sheet Source Surface (CSSS)model and the Potential Field Source Surface (PFSS) model,with the aim of determining whether the CSSS modelrepresents the solar wind sources better than the PFSSmodel. For this, we obtained the root mean square errors(RMSEs) and the correlation coefficients between theobserved solar wind speed and that predicted by themodels, the ratio of RMSEs between the two models, and askill score. On average, the CSSS predictions are moreaccurate than the PFSS predictions by a factor of~1.6,taking RMS error as the metric of accuracy. The RMS errorsincreased as the solar cycle progressed towards maximumindicating the difficulty in modelling the corona as theglobal field becomes more complex. We also compared theWSA/ENLIL predictions for a few Carrington rotations; WSAmodel makes use of the PFSS extrapolations to model thewind source. We found that the average value of RMSE ratiobetween the CSSS and the WSA/ENLIL predictions wasabout~1.9, implying that the CSSS predictions are nearlytwice better than the WSA/ENLIL predictions, despite thesimplicity of the CSSS model compared to ENLIL. Weconclude, based on the present analysis, that the CSSSmodel is a valid proxy for solar wind measurements andthat it improves upon existing commonly--used methods ofwind prediction or proxy analysis.Author(s): Bala Poduval (Southwest Research Institute), XuepuZhao (Stanford University)

323.61 – Interpretation of Solar SpectralIrradiance variations from analysis of 3DMHD simulationsRecent measurements by SIM radiometers show that thesolar irradiance varies in the Visible and IR bands incounterphase with the magnetic activity cycle. Suchvariations have been largely debated, as they do not agreewith measurements obtained with other radiometers, whilethe majority of reconstruction techniques employed toreconstruct the total irradiance do not reproduce suchsignals. It is therefore yet not clear whether the SIMmeasurements are still not fully compensated for residualinstrumental degradation, or if instead new physicalphenomena must be invoked to explain such variations. Alarge part of reconstruction techniques employsemiempirical one-dimensional models. In this contributionI will explain the limitations of such models and why weexpect a noticeable improvement of reconstructionsobtained by 3-D magnetohydrodynamic simulations. I willalso present some preliminary results obtained with theSTAGGER simulations which indicate that solar irradiance inthe Visible and IR bands might be in counterphase with themagnetic activity, as measured by SIM radiometers.Author(s): Serena Criscuoli (AURA-NSO)

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323.62 – A 3D Radiative Transfer Simulationof Lyma-alpha Backscatter IntensityReduced From Voyager’s UltravioletSpectrometerModels of the heliosphere have evolved for the past fewdecades to fit observations made by a large number ofspacecraft. Voyager missions have provided unique in-situmeasurements that have proven to be essential for modeltesting. Lyman-alpha backscatter intensity has beenreduced from measurements taken by the ultravioletspectrometers on board both Voyager spacecraft. We havedeveloped a 3D Monte Carlo radiative transfer code tosimulate this backscatter intensity by generating millions ofphotons from the sun to scatter within a neutral hydrogendistribution resulting from a state-of-the-art 3D MHD-kineticneutral heliospheric model, both of which have beendeveloped within the Center for Space Physics andAeronomic Research at the University of Alabama inHuntsville. While many have attempted to simulate theVoyager observations, we are the first to achieveagreement with our results. In this presentation, we willdiscuss the core mechanisms driving the radiative transfercode, the statistical quantities collected, and theinterpretation of the results relative to the spacecraft data.Author(s): Brian Fayock (University of Alabama in Huntsville), GaryZank (University of Alabama in Huntsville), Jacob Heerikhuisen (Universityof Alabama in Huntsville)

323.63 – The Turbulent Origin of the SlowSolar WindWe report on preliminary analyses of early solar windturbulence via heliospheric imaging: both the brightnessstructure function in the STEREO-A HI-1 field of view andpaths taken by individual boli of comet-tail material in thesolar wind. The analyses are complementary andpreliminary results indicate that turbulent processing isunderway even within the early HI-1 field of view (as low as20-30 Rs).Author(s): Craig DeForest (Southwest Research Inst.), BillMatthaeus (University of Delaware), Tim Howard (Southwest ResearchInst.)

323.64 – Connecting the Dots - MagneticField in the Inner HeliosphereAt any given time the Earth is connected by a cluster ofmagnetic field lines to the solar photosphere. The sameholds true for any location in the heliosphere - be it a solarorbiting spacecraft, region of particle acceleration, sourceof southward IMF, flare site, ICME, co-rotating interactionregion, comet, planet, etc. That cluster of field lines mayhave a common origin that is relatively easy to identify,e.g. in the center of a high speed stream originating in anequatorial coronal hole. More often the geometry iscomplex - adjacent field lines may come from widelyseparated places, the coronal topology may be convoluted,and the field will have been distorted during its transit.Furthermore, conditions change and history is important -foot points move or reconnect, the corona is dynamic -sometimes dramatically so, and the prior state of theheliosphere matters. Conversely, a region of interest, e.g.an active region, coronal hole, reconnection site, or shock,may be linked simply or in a more complex way to one ormany other locations in the heliosphere. We bring togethera variety of coronal and heliospheric modeling tools andnew sources of comprehensive solar data to improve theknowledge of how points in the heliosphere are connectedto each other and to the photosphere and how thoseconnections evolve in time. Our goal is to determine notonly the useful magnetic connections in the corona andinner heliosphere, but the implications of the corona'sfundamental skeletal structure for understanding sources ofin situ observations.Author(s): Jon Hoeksema (Stanford University), Yang Liu (StanfordUniversity), Xudong Sun (Stanford University), Aimee Norton (StanfordUniversity)

323.65 – Case Studies of InterplanetaryCoronal Mass EjectionsWe contrast the solar wind characteristics and origins fortypical and extreme ICME cases using STEREO data. Thispast solar minimum was characterized by weak transients.In contrast the rise of the cycle included extremely fastinterplanetary coronal mass ejections, with one such ICMEobserved in situ by STEREO A exceeding 1500 km/s at 1AU. We will compare specific cases of slow and fast ICMEsolar wind observed in situ by STEREO to general solar windion parameters, particularly for proton, helium and ironions.Author(s): Antoinette Galvin (Univ. of New Hampshire), KristinSimunac (Univ. of New Hampshire), Charles Farrugia (Univ. of NewHampshire)

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323.66 – Temporal Evolution of Solar WindIon Composition and their Source CoronalHoles During the Declining Phase of Cycle23We present our analysis of the temporal trend in the solarwind (SW) ion charge states and the properties in theassociated source coronal holes (CHs) during the decliningphase of solar cycle 23. We find that the SW ions exhibit atrend of decreasing ionization state with time, consistentwith previous studies. However the rate of decrease isdifferent between the slow and fast SW. The photosphericmagnetic field strength in both regions is found to exhibitsimilar trend of decrease with time. On the other hand, thetemporal trend is different in the line emissions fromdifferent layers of the atmosphere (chromosphere, transitregion and corona). Within each CH, the coronal emissiongenerally increases toward the boundary of the CH as theunderlying photospheric magnetic field strength increases,the net unbalanced field strength decreases and themagnetic field becomes less unipolar. But the coronalemission averaged over the entire CH area does not haveappreciable change with time. We find that ions whichfreeze-in at lower altitude in the corona, such as C and Oions, have a stronger correlation between their ionizationstate and the average photospheric magnetic field strengthin the slow SW, while Fe ions which freeze-in at higheraltitude have a stronger correlation in the fast SW. Ouranalyses provide important clues for how the SW is formed,heated and accelerated in response to the long-termevolution of the solar magnetic field at its source coronalhole.Author(s): Yuan-Kuen Ko (Naval Research Laboratory), KarinMuglach (NASA Goddard Space Flight Center), Yi-Ming Wang (NavalResearch Laboratory), Peter Young (George Mason University), Susan Lepri(University of Michigan)

323.67 – A Study of Type II Radio Bursts toMap the Alfvén Speed Profile in the InnerHeliosphereIt is well accepted that interplanetary Type II radio burstsare the manifestations of electron acceleration in shocksdriven by propagating of coronal mass ejections (CMEs)traveling faster than the characteristic local fastmagnetosonic speed. A prominent feature of type II radiobursts is the intermittency of the observed emission acrossthe metric, decametric and kilometric frequency ranges, asthe shock propagates to greater distances. This can beattributed to changes in both the shock driver and to theconditions in the ambient medium. We present results froma survey of coronal and interplanetary type II radio burstsusing radio observations from STEREO/WAVES andWIND/WAVES to determine the distance of the observedtype II emission and the speed of the associated shock. Byestablishing regions of the corona and interplanetarymedium that are predisposed to shock formation, we mapout the profile of the fast magnetosonic speed, and in turninfer the local Alfvén speed.Author(s): Hazel Bain (University of California, Berkeley), JuanCarlos Martinez Oliveros (University of California, Berkeley), DavidSundkvist (University of California, Berkeley), Stuart Bale (University ofCalifornia, Berkeley)

323.68 – A Survey of STEREO LET SEPAnisotropies and their Solar andHeliospheric AssociationsStudies have shown solar energetic particle (SEP) eventsdisplay a variety of anisotropy behaviors. The Low-EnergyTelescope (LET) of the IMPACT SEP instrument onboard theSTEREO spacecraft provides in situ angular distributionmeasurements of the 4 – 6 MeV SEP proton flux. Using theinstruments sunward and antisunward-facing sectoreddetector, we survey anisotropies present in SEP eventscovering the LET observing period. The events arecategorized into those associated with unidirectional,bidirectional and omnidirectional pitch angle distributionsand classified in accordance with their relation to ICMEshock and magnetic cloud signatures. Determination of thesource origin from the east or west of the Sun adds contextfor our understanding of these events.Author(s): Hazel Bain (University of California, Berkeley), JanetLuhmann (University of California, Berkeley), Yan Li (University ofCalifornia, Berkeley), Richard Leske (California Institute of Technology),Leila Mays (NASA/GSFC)

323.69 – Role of Heliospheric MagneticMirrors in Major SEP EventsOne of the challenges in interpreting major solar energeticparticle (SEP) events is that they often occur when multipleCMEs occur - making the distinction between what is newlyinjected at the shock source and what is temporarilytrapped in the disturbed heliospheric field difficult tountangle. Recent ENLIL heliospheric modeling of suchcomplex CME periods, including the major events periods ofMarch 2012 and July 2012, provide some first-orderindications of possibly existing SEP magnetic traps andtheir influences. For example, one can examine themagnetic field strength along field lines to find local minimain the field -from which trapping efficiencies can beevaluated from conservation of adiabatic invariants. Onecan also determine the spatial extent and lifetimes of thesetraps. The results give an idea of how important the largescale magnetic geometry can be in determining theheliospheric SEP environment- especially at very activetimes. Models that do not take this into account mayincorrectly infer the shock source strength and timeevolution. (Model results provided by CCMC/SWRA.)Author(s): Janet Luhmann (UC, Berkeley), Leila Mays (CUA), DusanOdstrcil (George Mason University), Hazel Bain (UC, Berkeley), Yan Li (UC,Berkeley)

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323.70 – Laboratory Study of MagneticReconnection in Partially Ionized PlasmasRelevant to the Solar ChromosphereMagnetic reconnection is observed to occur in the solarchromosphere where plasma is only partially ionized. Inorder to understand the effects of partial ionization on thereconnection process, systematic experiments have beenperformed in the Magnetic Reconnection Experiment (MRX)where plasma is controlled from nearly full ionization topartial ionization of about 1%. It is shown that, whenneutrals are added, the Hall quadrupole field pattern andthus electron flow are unchanged while the ion outflowspeed is reduced due to ion-neutral drag. However, incontrast to theoretical predictions, the ion diffusion layerwidth does not change appreciably. Therefore, the total ion

outflow flux and the normalized reconnection rate arereduced*. Both 2-fluid and 3-fluid modeling using the HiFicode is used to interpret the experimental data, andimplications to the interpretation of solar observations willbe also discussed. Future plans to study effects of neutralparticles on further details on magnetic reconnection, suchas plasma heating, will be described. * E. Lawrence, H. Ji, M.Yamada, and J. Yoo, “Laboratory Study of Hall Reconnectionin Partially Ionized Plasmas”, Phys. Rev. Lett. 110, 015001(2013).Author(s): William Fox (Princeton Plasma Physics Laboratory), BartDe Pontieu (Lockheed Martin), Hantao Ji (Princeton Plasma PhysicsLaboratory), Eric Lawrence (Princeton Plasma Physics Laboratory),Vyacheslav Lukin (Naval Research Laboratory), Nicholas Murphy (Havard-Smithsonian Center for Astrophysics), Masaaki Yamada (Princeton PlasmaPhysics Laboratory), Jongsoo Yoo (Princeton Plasma Physics Laboratory)

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301 – On the Shoulders of Giants: Planets Beyond the Reach of Kepler III:Ground-based Imaging and SpectroscopyMeeting-in-a-Meeting – America Ballroom North/Central – 04 Jun 2014 10:00 AM to 11:30 AM

What kind of planets lie at orbit radii of 1-2 AU - beyond the reach of Kepler? In the last two decades we haveexplored a large sample of RV-detected and transit-detected planets, discovered distant planets with microlensingand several hot young planets at large radii using direct imaging, as well as the debris disks that provide clues toformation and evolution. In these 4 sessions, we explore the near future, and how we can expect to learn muchmore about the demographics and properties of cold outer planets. WFIRST-AFTA will open up this area, with amicrolensing survey to probe the population of long-orbit planets, and coronagraphy to take images and spectraof large planets in orbits at a few AU. Session III covers direct observation of exoplanets with imaging andspectroscopy, and what we learn from debris-disks around planet-bearing stars.

Chair(s):Charles Beichman (JPL)


301.01 – Detecting and CharacterizingExoplanets with Direct Imaging from theGroundThe last decade has yielded the first images of exoplanets,considerably advancing our understanding of the propertiesof young giant planets. In this talk I will discuss currentresults from ongoing direct imaging efforts as well as futureprospects for detection and characterization of exoplanetsvia high contrast imaging. Direct detection, and directspectroscopy in particular, have great potential foradvancing our understanding of extrasolar planets. Incombination with other methods of planet detection, directimaging and spectroscopy will allow us to eventually: 1)study the physical properties of exoplanets (colors,temperatures, etc.) in depth and 2) fully map out thearchitecture of typical planetary systems. Direct imaginghas offered us the first glimpse into the atmosphericproperties of young high-mass (3-10 M Jup ) exoplanets.Deep direct imaging surveys for exoplanets have alsoyielded the strongest constraints to date on the statisticalproperties of wide giant exoplanets.Author(s): Beth Biller (MPIA)

301.02 – The Gemini Planet ImagerThe Gemini Planet Imager (GPI) is a next-generationadaptive optics coronagraph designed for direct imagingand spectroscopy of extrasolar planets and polarimetry ofcircumstellar disks. It is the first such facility-classinstrument deployed on a 8-m telescope, designed toachieve contrast levels of up to 10^7. This allowsobservations of warm self-luminous planets, with massesgreater than a Jupiter mass and ages less than a fewhundred megayears. GPI will be used for a large-scalesurvey of 600 nearby young stars, as well as for guestobserver science. I will present first-light science resultsand discuss the scientific capabilities of GPI.Author(s): Bruce Macintosh (Stanford University)

301.03 – SEEDS - Direct Imaging ofExoplanets and Their Forming Disks withthe Subaru TelescopeSEEDS (Strategic Explorations of Exoplanets and Disks withSubaru) is the first Subaru Strategic Program, whose aim isto conduct a direct imaging survey for giant planets as wellas protoplanetary/debris disks at a few to a few tens of AUregion around 500 nearby solar-type or more massiveyoung stars devoting 120 Subaru nights for 5 years. Thetargets are composed of five categories spanning the agesof ~1 Myr to ~1 Gyr. Some RV-planet targets with olderages are also observed. The survey employs the newhigh-contrast instrument HiCIAO, a successor of theprevious NIR coronagraph camera CIAO for the SubaruTelescope. More than 100 nights have already beenobserved so far without major instrument troubles. Wedescribe the outline of this survey and present its mainresults. The topic includes (1) detection andcharacterization of one of the most lowest-mass planet viadirect imaging. (2) detection of a super-Jupiter around themost massive star ever imaged, (3) detection ofcompanions around retrograde exoplanet, which supportsthe Kozai mechanism for the origin of retrograde orbit. Wealso report (4) the discovery of unprecedentedly detailedstructures of more than a dozen of protoplanetary disks andsome debris disks. The detected structures such as widegaps and spirals arms of a Solar-system scale could besignpost of planet.Author(s): Motohide Tamura (National Astronomical Obs.)

Contributing teams: SEEDS team

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301.04 – Tracing Planetary SystemArchitecture with Debris Disk ImagingPlanetary systems can be imaged indirectly via their debrisdisks - the remnants left over after planets form. Ongoingdestruction of asteroids and comets in these disks creates acontinual supply of orbiting dust around most Sun-likestars, including our own. In the Solar System such dust isbright enough to be seen with the naked eye - the Zodiacallight. Far-infrared observations by the Spitzer SpaceTelescope and the Herschel Space Observatory haveidentified many nearby stars with even brighter orbitingdebris, orders of magnitude more than in the Solar System.Because they are so bright, optical imaging of debris disksis much easier than detecting their embedded planets.Such planets can be inferred from disk structure - the innerwarp of beta Pic and the sharply defined eccentric rings ofFomalhaut and HD 202628, for example. Resolvingindividual belts of debris, meanwhile, infers the location ofintermediate planets (as in the HR 8799 planetary system)and allows for comparison with the 2-belt architecture ofSolar System. Debris disk imaging is particularly well suitedtoward exploring the outer regions of planetary systems(>10 AU), where mature (cold) planets cannot otherwise bedetected. Overall, images of debris disks probe theirunderlying planetary systems both generally, by mappingthe system architecture, and specifically, by determiningthe location of individual planets.Author(s): Geoffrey Bryden (JPL)

301.05 – Overview of future ground andspace imaging capabilitiesThis talk serves as an introduction to the session andcontext of future exoplanet direct imaging capabilities onthe ground and in space. The emphasis of the presentationis on short-medium term. On the ground a new generationof instrument (Gemini Planet Imager, VLT-SPHERE, MagellanAO) are beginning their operations with considerableimprovement over the previous capabilities. In space, whileHST continues operations and provides high-contrastcapabilities, JWST will offer several coronagraphs both onthe NIRCam and MIRI instrument as well as an aperturemasking mode on NIRISS. The possibility of a coronagraphyon WFIRST/AFTA also opens new possibilities forspace-based coronagraphy in the medium term.Author(s): Remi Soummer (Space Telescope Science Institute)

301.06 – Pushing the radial velocityaccuracy of HARPS and HARPS-N.HARPS and HARPS-N are reaching an incredible radialvelocity precision of one meter per second on bright stars.This precision is made possible by the stability of theinstrument, and the cross correlation technique thataverages out the different sources of noise by stackingtogether the information of all the observed spectral lines.All possible lines in the spectrum are used, except a fewlines sensitive to activity like for example the Ca II H and Klines, and lines close to telluric features. However, thespectra are recorded on a CCD that is not perfect. With theEarth rotating around the Sun, the spectra are shifted backand forth on the CCD and spectral lines are recorded ondifferent sets of pixels as a function of time. I will showsome strange behavior of spectral lines that crosses knownfeatures on the CCD. Some specific lines show hundreds ofmeters per second variation on stars that we know arequiet at the meter per second level. By studying the RVvariation of each line as a function of time and notconsidering the ones that exhibit strong variations, it ispossible to improve the accuracy of the measurementstaken by HARPS and HARPS-N. I will show that this reducesthe noise in the RV measurements, which allows us toconfirm or reject some planetary detections that are at thelimit of the noise.Author(s): Xavier Dumusque (Harvard Smithsonian CfA)

301.07 – First science results from the K2missionThe K2 mission expands upon Kepler's groundbreakingdiscoveries in the fields of exoplanets and astrophysicsthrough new and exciting observations. K2 will use aninnovative way of operating the spacecraft to observetarget fields along the ecliptic for the next 2-3 years. Earlyscience commissioning observations have shown anestimated photometric precision near 400 ppm in a single30 minute observation, and a 6-hour photometric precisionof 80 ppm (both at V=12). Here we present the first sciencedata from the spacecraft. These include observations oftransiting planets, eclipsing binaries and pulsating stars.Author(s): Thomas Barclay (NASA Ames Research Center)

Contributing teams: The K2 Mission team

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302 – Chromosphere and Transition Region IMeeting-in-a-Meeting – America Ballroom South – 04 Jun 2014 10:00 AM to 11:30 AMChair(s):Holly Gilbert (NASA's Goddard Space Flight Center)

302.01 – Chromospheric Diagnostics fromIRIS and DSTUsing data obtained during a coordinated observingcampaign in September 2013, we compare the spectral andimaging diagnostics from IRIS and the instruments at theDunn Solar Telescope (DST). We focus on a small activeregion observed for approximately one hour with IRIS (NUV,FUV, and SJI) in conjunction with IBIS, FIRS, and ROSA fromthe DST. In particular, we examine the line widths andintensities in the different chromospheric lines (H-alpha, CaII 8542, Mg II) and the temporal evolution of these differentdiagnostics. This allows us to better relate the views fromnew window provided by IRIS to previous studies of thechromosphere.Author(s): Gianna Cauzzi (National Solar Observatory), KevinReardon (INAF), Sarah Jaeggli (Montana State University), Aaron Reid(Queen's University Belfast)

302.02 – Intense active region brighteningsobserved by IRISActive region raster scans obtained with the InterfaceRegion Imaging Spectrometer (IRIS) typically reveal a fewextremely intense brightenings in the Si IV emission lines(formed around 80,000 K) that are not related to flares. Thebrightenings are around 0.5-1.0 arcsec (0.4-0.8 Mm) in size,and the line profiles can be very broad (up to 300 km/s),showing multiple emission components. Similarbrightenings were reported from the Coronal DiagnosticSpectrometer (CDS) on board the Solar and HeliosphericObservatory (SOHO) and were termed active regionblinkers. The much higher spatial and spectral resolution ofIRIS together with high cadence coronal and photosphericimaging from the Solar Dynamics Observatory allows thebrightenings to be identified with magnetic field andcoronal signatures. Example events will be shown andstatistics given.Author(s): Peter Young (George Mason University)

302.03 – The role of the chromosphere inthe energization of the corona.We present results on the effect of the partially ionizedchromosphere on the transfer of magnetic field and energyinto the corona during the birth and evolution of solaractive regions. Using numerical MHD simulations whichinclude the effects of partial ionization, namely ion-neutralcollisions and Pedersen dissipation, we investigate how themagnetic flux and energy emerges from beneath thssurface to energize the corona, and how thesechromospheric partial ionization effects modulate theseprocesses. Of particular interest is the nature of the electriccurrents and the force-free nature of the magnetic field.Author(s): James Leake (George Mason University), Mark Linton(Naval Research Laboratory)

302.04 – From static to dynamic mapping ofchromospheric magnetism - FIRS and SPIESAdvancements in theoretical forward modeling andobservational techniques now allow the mapping of thechromospheric magnetic field vector in some regions. Wereport on full maps of the chromospheric magnetic fieldvector across a sunspot and its superpenumbra withinNOAA AR 11408. These maps are derived from full Stokesobservations of the He I triplet at 1083 nm, which showboth Zeeman and atomic-level polarization signatures. Yet,due to the long time to acquire these observations with theslit-based Facility Infrared Spectropolarimeter (FIRS), ourmeasurements primarily probe long-lived chromosphericstructures, albeit at very high polarization sensitivity. Thefast temporal scales remain difficult to probe withconventional slit-based spectropolarimeters. Alternatively,SPIES is an instrument based on a birefringent fiber opticIFU, designed to multiplex a two-dimensional spatial fieldwith high spectral resolution spectropolarimetry, and is anideal tool for probing small-scale, dynamic magneticfeatures. We will present movies of the dynamicchromosphere acquired from SPIES across a sunspot and itsfine-scaled superpenumbra.Author(s): Thomas Schad (University of Hawaii), Haosheng Lin(University of Hawaii)

302.05 – First Simulations of a CollisionalTwo-Stream Instability in the ChromosphereObservations and modeling shows that immediately abovethe temperature minimum in the solar atmosphere, a steeprise from below 4,000 K to over 6,000K occurs. Recentpapers show that a collisional two-stream plasma instabilitycalled the Farley-Buneman Instability can develop at thealtitudes where this increase occurs. This instability mayplay an important role in transferring energy from turbulentneutral flows originating in the photosphere to themid-chromosphere in the form of heat. Plasma turbulenceresulting from this instability could account for some ormost of this intense chromospheric heating. This paperpresents a set of simulations showing the development andevolution of the Farley-Buneman Instability (FBI) applicableto the chromosphere. It compares these results with thebetter-understood ionospheric FBI. It examines the linearbehavior and the dependence of growth rates for a range ofaltitudes and driving flows. It also presents the first study ofFBI driven plasma nonlinearities and turbulence in thechromosphere. This research should help us evaluate theFBI as a mechanism to convert neutral flow and turbulenceenergy into electron thermal energy in the quiet Sun.Author(s): Meers Oppenheim (Boston University), Yakov Dimant(Boston University), Chad Madsen (Boston University), Juan Fontenla(Northwest Research Institute)

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302.06 – Chromospheric NanoflaresThe traditional view is that coronal plasma results fromenergy release (reconnection, waves, etc.) that takes placeabove the chromosphere, in the corona itself. However, thisneed not be the case. Cool chromospheric plasma could bedirectly heated to high temperatures and rise upward to fillthe corona. We here investigate this scenario in the contextof impulsive nanoflares that occur in the upperchromosphere. Such events could represent the suddenheating of the tips of type II spicules, or they could takeplace in the ordinary chromosphere, completely unrelatedto spicules. The results are general. We generate synthetic

line profiles of Fe XIV (274) and Fe XII (195) based on aseries of simulations performed with the HYDRAD 1D hydrocode, which includes non-equilibrium ionization. We findthat the profiles are strongly blue-shifted and/or have largeasymmetries that are grossly inconsistent with actualobservations. The results are in agreement with ourprevious analytical predictions (Klimchuk 2012). Weconclude that most coronal plasma is a result of coronalenergy release, not chromospheric nanoflares or type IIspicules.Author(s): James Klimchuk (NASA GSFC), Stephen Bradshaw (RiceUniversity)

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303 – CME IIMeeting-in-a-Meeting – Staffordshire – 04 Jun 2014 10:00 AM to 11:30 AMChair(s):Thomas Berger (Lockheed Martin Adv. Tech. Ctr.)

303.01 – A Topological View at ObservedFlare Features: An Extension of theStandard Flare Model to 3DWe conduct topology analysis of erupting non-linearforce-free field (NLFFF) configurations of eight sigmoidalactive regions observed with Hinode/XRT and SDO/AIA. TheNLFFF models are computed using the flux rope insertionmethod and unstable models are utilized to represent theerupting configurations. Topology analysis shows that thequasi-separatrix layers (QSLs) in the chromosphere matchwell the flare ribbons observed in these regions. In addition,we show that low-lying QSLs associated with the rising fluxrope change shape and extent to match the separatingflare ribbons as observed by AIA. Post-flare loops are fit wellby field lines lying under the generalized X-line at thebottom of the flux rope. We show a correspondence in theevolution of the post-flare loops from a strong-to-weaksheared state and the behavior of the field lines as the fluxrope expands in the corona. We show that transient coronaholes are associated with the footprints of the flux rope inthe low atmosphere. In addition, we compute thereconnected flux in one of the regions and usinginformation from the models constrain how much energyhas been released during the event. We use this kind oftopology analysis to extend the standard CME/flare modelto full 3D and find implications to reconnection in 3D.Author(s): Antonia Savcheva (Harvard-Smithsonian Center forAstrophysics), Etienne Pariat (Paris Observatory, Meudon), Sean McKillop(Harvard-Smithsonian Center for Astrophysics), Elizabeth Hanson (Univ. ofCalifornia, Berkley), Yingna Su (Harvard-Smithsonian Center forAstrophysics), Edward DeLuca (Harvard-Smithsonian Center forAstrophysics)

303.02 – Kelvin-Helmholtz instability drivenby CMEs expanding in a turbulent mediumRecent high resolution AIA/SDO images show clearevidence of the development of the Rayleigh-Taylorinstability, as coronal mass ejections (CMEs) expand in theambient corona. A large-scale magnetic field mostlytangential to the interface is observed, both on the CMEand on the background sides. However, this magnetic fieldis not intense enough to quench the instability. The ambientcorona is expected to be in a turbulent regime, andtherefore the development of the Raleigh-Taylor instabilitycan significantly differ from the one corresponding to alaminar medium. To study the evolution of the Rayleigh-Taylor instability in a turbulent background, we performthree-dimensional simulations of themagnetohydrodynamic equations. The instability is drivenby a velocity profile tangential to the CME-corona interface,which we simulate through a hyperbolic tangent profile.The turbulent background is obtained by the application ofa stationary stirring force. One of the outcomes of thesesimulations is the computation of the instability growth-ratefor different values of the correlation length of theturbulence.Author(s): Daniel Gomez (IAFE), Edward DeLuca (Harvard-SmithsonianCenter for Astrophysics), Pablo Mininni (University of Buenos Aires)

303.03 – A SOLAR ERUPTION DRIVEN BYRAPID SUNSPOT ROTATIONWe present the observation of a major solar eruption that isassociated with fast sunspot rotation. The event includes asigmoidal filament eruption, a coronal mass ejection, and aGOES X2.1 flare from NOAA active region 11283. Thefilament and some overlying arcades were partially rootedin a sunspot. The sunspot rotated at $\sim$10$^\circ$ perhour rate during a period of 6 hours prior to the eruption. Inthis period, the filament was found to rise gradually alongwith the sunspot rotation. Based on the HMI observation,for an area along the polarity inversion line underneath thefilament, we found gradual pre-eruption decreases of boththe mean strength of the photospheric horizontal field($B_h$) and the mean inclination angle between the vectormagnetic field and the local radial (or vertical) direction.These observations are consistent with the pre-eruptiongradual rising of the filament-associated magneticstructure. In addition, according to the Non-Linear Force-Free-Field reconstruction of the coronal magnetic field, apre-eruption magnetic flux rope structure is found to be inalignment with the filament, and a considerable amount ofmagnetic energy was transported to the corona during theperiod of sunspot rotation. Our study provides evidencesthat in this event sunspot rotation plays an important rolein twisting, energizing, and destabilizing the coronalfilament-flux rope system, and led to the eruption. We alsopropose that the pre-event evolution of $B_h$ may be usedto discern the driving mechanism of eruptions.Author(s): Yao Chen (Institute of Space Sciences), Guiping Ruan(Institute of Space Sciences)

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303.04 – The Relation between Type II RadioBursts and Large-scale Coronal PropagatingFrontsBoth type II radio bursts and chromospheric Moreton-Ramsey waves are believed to signify shock waves thatpropagate in the solar corona. Large-scale coronalpropagating fronts (LCPFs), which are also called EIT waves,EUV waves or coronal bright fronts in the literature, wereinitially thought to be coronal counterparts of Moreton-Ramsey waves, and thus they were expected to becorrelated with type II bursts. At present, the prevailingview seems to be that both type II bursts and LCPFs aremore closely linked with CMEs than with flares. Here werevisit the relation between type II bursts and LCPFs, byexamining radio dynamic spectra (180-25 MHz) as obtainedby USAF/RSTN and analyzing EUV and white-light data fromSDO and STEREO. In the sample of about 140 type II burstsand LCPFs between April 2010 and January 2013, we findthe correlation of 50-60 %. Type II bursts could beassociated with eruptions without significant lateralexpansion, and fast LCPFs could show no presence in themetric radio spectral range. Using data from STEREO COR-1that observed the CME as a limb event, in 42 cases wedirectly measure the height of the CME at the onset of thetype II burst. As expected, the height tends to be lowerwhen the type II burst starts at a higher frequency. It isfound that those type II bursts that start at higher altitudesand lower frequencies tend to have weaker EUV fronts. Thismay indicate multiple ways of how LCPFs and type II burstsare related with CMEs.Author(s): Nariaki Nitta (Lockheed Martin, ATC)

303.05 – Do all CMEs deflect to thebackground magnetic minimum by 4Rs?Accurate space weather forecasting requires knowledge ofthe trajectory of coronal mass ejections (CMEs), includingany CME deflection close to the Sun or throughinterplanetary space. Kay et al. (2013) introduced ForeCAT,a model of CME deflection resulting from the backgroundsolar magnetic field. For a magnetic backgroundcorresponding to Carrington Rotation (CR) 2029 (decliningphase, April-May 2005), the majority of the CMEs deflectedto the streamer belt, the minimum in magnetic pressure.Most of the deflection occurred below 4 Rs. Here we explorethe questions: a) Do all CMEs deflect to the magneticminimum? and b) Does most deflection occur within 4 Rs?We have eliminated many of the underlying simplificationsof ForeCAT presented in Kay et al. (2013) with a moredetailed three dimensional description of the deflecting fluxrope. The locations of coronal magnetic structures thatdetermine the background magnetic minima varythroughout the solar cycle. We show that these variationsreproduce observed trends in the direction of CMEdeflections throughout the solar cycle.Author(s): Christina Kay (Boston Univ.), Merav Opher (Boston Univ.)

303.06 – Are Polar-crown Coronal MassEjections Similar to the Low-latitudeCounterparts?Coronal mass ejections (CMEs) from the polar-crownfilament region originate above 60-degree latitude duringsolar activity maxima. Polar-crown CMEs originate frombipolar magnetic regions, whereas both bipolar andmultipolar regions produce CMEs at low latitudes. If polarCMEs are similar to the low-latitude ones, then a singleeruption mechanism can apply to all CMEs, the commonelement being the magnetic free energy. We examineseveral polar-crown CMEs to determine their three-partmorphology, acceleration profile including the height ofpeak acceleration, CME-flare relationship, and energetics.We found that these properties are similar to those oflow-latitude CMEs. We use illustrative examples from theSolar Dynamics Observatory images to show quantitativelythat the polar-crown CMEs are very similar to theirlow-latitude counterparts. Even though the post eruptionarcades are weak, we show that the peak thermal energy ofthese arcades is a few percent of the CME kinetic energy,similar to what is observed in large eruptive events. Theseobservations suggest that a bipolar configuration issufficient for the production of CMEs.Author(s): N. Gopalswamy (NASA GSFC), Seiji Yashiro (NASA GSFC),Sachiko Akiyama (NASA GSFC)

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304 – Observation and Theory for MultiverseSpecial Session – St. George AB – 04 Jun 2014 10:00 AM to 11:30 AM

The multiverse is a hypothetical set of finite or infinite possible universes existing in the entire space. The highlyprecise map of cosmic microwave background (CMB) radiation from the data recently measured by the Plancksatellite has shown some anomalies that give a hard evidence for the multiverse. The standard big bang universemodel predicts that the cosmic microwave background radiation of the universe should be evenly distributed, butthe map shows a stronger concentration or hotter in the south half of the sky and a large colder spot that is alsonot understandable under conventional physics. In addition, the observation of quantum nonlocality and thetheory of natural unnaturalness have also provided support or evidence for the multiverse. There are variousmultiverse models developed so far such as the bubble universe model. Max Tegmark categorized the variousmultiverse models as four levels, while Brian Greene divided them into nine typ es. Recently, Tianxi Zhang slightlymodified the standard big bang theory and developed a new multiverse model called black hole universe, which isconsistent with Mach’s principle, governed by Einstein’s genera relativity, and be able to explain all observationsof the universe. It has only one postulate but can self-consistently interpret the origin, structure, evolution, andexpansion as well as quantitatively explain the measurements for the redshift and luminosity distance of type-Iasupernovae, the cosmic microwave background radiation, and the emissions of quasars and gamma-ray bursts.This session is proposed to the 224th AAS meeting in order for cosmologists to discuss and share their recentinvestigations on the multiverse theories and observations.

Chair(s):Tianxi Zhang (Alabama A&M University)

304.01 – Experimentally Testing theMulitverse/Many-Worlds TheoryMany-Worlds quantum mechanics is NOT experimentallyequivalent to standard quantum mechanics. I shalldemonstrate this fact and investigate its consequences. Ifirst show the Schrödinger equation is a special case of the

classical Hamilton-Jacobi equation, with |?|2 being mostnaturally interpreted as a quantity proportional to thedensity of universes in the multiverse. I then show that with

this interpretation for |?|2, we can test the multiversetheory, because in the multiverse theory, the BornInterpretation is derived from this assumption, not merelyassumed as in standard quantum theory, and the

derivation gives us a means of computing how fast |?|2 willbuild up from individual particles in an experiment, acomputation I shall show cannot be done in standardquantum mechanics. In some types of experiments, theobserved pattern will approach the final Born pattern as

1/N1/2, and in other types of experiments, the approach willbe as 1/N, where N is the number of observed “particles.”The multiverse meaning of has other advantages over thestandard probability amplitude meaning, because if is auniverse density amplitude, need not be restricted to beinga Hilbert space function. In particular, delta functions andplane waves are NOT functions in any Hilbert space, butthey are both used extensively in quantum mechanics,though disallowed by the axioms of standard quantummechanics. Finally, I shall show that multiverseexperiments have important implications for cosmology.The Wheeler-DeWitt equation for quantum gravity, appliedto a spatially closed Friedman radiation universe inconformal time, is mathematically the Schrödinger equationfor a simple harmonic oscillator. I show that if the wavefunction of the universe were a delta function at the initialsingularity — I show that the universes being exactlyclassical now implies such a universal wave function —then we are overwhelmingly likely to find ourselves in aclosed universe that is very large, hence nearly flat. Thusthe existence of the multiverse solves the FlatnessProblem. No inflation force is needed. I show ALL majorproblems of cosmology can be similarly solved.Author(s): Frank Tipler (Tulane University)

304.02 – Testing Quantum Mechanics andBell's Inequality with CosmologicalObservations of QuasarsWe discuss a proposed experiment which would leveragecosmology to test quantum mechanics using astronomicalobservations. Specifically, we aim to close the "settingindependence" or so-called "free will" loophole inexperimental tests of Bell's inequality by choosing thedetector settings (e.g. polarizer orientations) usingreal-time observations of causally disconnected cosmicsources, for example sufficiently distant quasar pairs, allwhile the entangled particles are still in flight. This wouldhelp close one of the most important remaining Bell testloopholes whereby an alternative theory could mimic thequantum predictions if the experimental settings choicesshared even a small correlation with some local "hiddenvariables" due to unknown causal influences a mere fewmilliseconds prior to the experiment. Our "Cosmic Bell"experiment would push any such hidden variableconspiracy all the way back to the hot big bang 13.8 Gyrago, an improvement of 20 orders of magnitude. The talkwill demonstrate the real world feasibility of ourexperimental setup, with emphasis on the theoreticalcosmology constraints needed to choose optimal sources.We thus describe general conditions for pairs ofcosmological events with arbitrary redshifts and angularseparations to have no shared causal pasts since the hotbig bang in flat, dark energy dominated, acceleratingFriedman-Lemaitre-Robertson-Walker universes like ourown. While causally disjoint patches of the cosmicmicrowave background radiation at redshift z ~ 1090 couldbe used to set the detectors, z > 3.65 quasars observed atoptical wavelengths are arguably the optimal candidatesource pairs using present technology that meet thecondition of having no shared causal past since the end ofany period of inflation, 13.8 Gyr ago. Results are illustratedfor our universe with causal structure animations to helpvisualize the intersections of past light cones for arbitraryevent pairs.Author(s): Andrew Friedman (Harvard-Smithsonian Center forAstrophysics), Jason Gallicchio (University of Chicago, Kavli Institute forCosmological Physics), David Kaiser (Massachussetts Institute ofTechnology, Center for Theoretical Physics), Alan Guth (MassachussettsInstitute of Technology, Center for Theoretical Physics)

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304.03 – The Black Hole Universe ModelThe black hole universe model is a multiverse model ofcosmology recently developed by the speaker. According tothis new model, our universe is a fully grown extremelysupermassive black hole, which originated from a hotstar-like black hole with several solar masses, and graduallygrew up from a supermassive black hole with million tobillion solar masses to the present state with trillion-trillionsolar masses by accreting ambient matter or merging withother black holes. The entire space is structured withinfinite layers or universes hierarchically. The innermostthree layers include the universe that we live, the insidestar-like and supermassive black holes called childuniverses, and the outside space called mother universe.The outermost layer is infinite in mass, radius, and entropywithout an edge and limits to zero for both the matterdensity and absolute temperature. All layers are governedby the same physics and tend to expand physically in onedirection (outward or the direction of increasing entropy).The expansion of a black hole universe decreases itsdensity and temperature but does not alter the laws ofphysics. The black hole universe evolves iteratively andendlessly without a beginning. When one universe expandsout, a new similar one is formed from inside star-like andsupermassive black holes. In each of iterations, elements

are resynthesized, matter is reconfigurated, and theuniverse is renewed rather than a simple repeat. The blackhole universe is consistent with the Mach principle,observations, and Einsteinian general relativity. It has onlyone postulate but is able to explain all phenomena occurredin the universe with well-developed physics. The black holeuniverse does not need dark energy for acceleration and aninflation epoch for flatness, and thus has a devastatingimpact on the big bang model. In this talk, I will presenthow this new cosmological model explains the variousaspects of the universe, including the origin, structure,evolution, expansion, background radiation, acceleration,anisotropy, quasars, gamma-ray bursts, nucleosynthesis,etc., and compares to the big bang model.Author(s): Tianxi Zhang (Alabama A&M University)

304.04 – Are Parallel Universes UnscientificNonsense or Should BICEP2 Make Us TakeThem Seriously?Parallel universes are not theories, but predictions ofcertain theories, such as eternal inflation and no-collapsequantum mechanics. I explore the logical links betweenrecent experimental progress in cosmology and other areasand various types of parallel universes.Author(s): Max Tegmark (MIT)

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305 – Bridging Laboratory & Astrophysics: PlasmasMeeting-in-a-Meeting – St. George CD – 04 Jun 2014 10:00 AM to 11:30 AM

Laboratory astrophysics is the Rosetta Stone that enables astronomers to understand and interpret the cosmos.This session will focus on the interplay between astrophysics with theoretical and experimental studies into theunderlying plasma processes, which drive our Universe.

Chair(s):R. Paul Drake (Univ. of Michigan)Organizer(s):Farid Salama (NASA Ames Research Center)

305.01 – Using Laser-produced Plasmas toStudy Magnetized Collisionless ShocksA new laser experiment to study the interaction of anenergetic laser plasma with a large magnetized ambientplasma is now operational at the Large Plasma Device(LAPD) at UCLA. A rapidly exploding, and super-Alfvénic(MA>2) plasma-plume is created by irradiating a solidtarget within the preformed magnetized plasma with anenergetic laser pulse (200 J in 20 ns). The ambient plasma

(1013 cm-3, 5 eV) is current free, stationary, quiescent, andlarge enough (17x0.5 m) to support Alfvén waves. Thedynamics of the laser-plasma piston and formation andstructure of the shock is measured with magneticflux-probes, spectroscopy, and Thomson scattering. Weobserve how the initial magnetic pulse steepens into acollisionless shock and separates from the piston by severalion Larmor radii. Hybrid simulations indicate that thesefeatures can be directly related to the degree ofcollisionless plasma coupling. The results will be discussedin the context of debris-ambient coupling in space andastrophysical explosions and other laboratory experiments.Author(s): Christoph Niemann (UCLA), Derek Schaeffer (UCLA), ErikEverson (UCLA), E. Clark (UCLA), Anton Bondarenko (UCLA), CarmenConstantin (UCLA), Walter Gekelman (UCLA), Dan Winske (Los AlamosNational Laboratory)

305.02 – Progress In Iron TransmissionMeasurements Relevant to the SolarConvection/Radiation BoundaryIron plasma opacity influences the internal structure of thesun. However, opacity models have never beenexperimentally tested at stellar interior conditions. Recentiron opacity experiments at the Sandia Z facility reached195 eV temperatures, nearly the same as the solarconvection/radiation zone boundary (CZB), at electrondensities that are roughly ½ the solar CZB value. Progressto solidify these results and use them to examine thephysical underpinnings of opacity models will be described.We will also discuss impact of the results on the Rosselandmean opacities important for stellar physics.++Sandia is amultiprogram laboratory operated by Sandia Corporation, aLockheed Martin Company, for the United StatesDepartment of Energy under contract DE-AC04-94AL85000.Author(s): Jim Bailey (Sandia National Laboratories), T. Nagayama(Sandia National Laboratories), G. Loisel (Sandia National Laboratories), G.Rochau (Sandia National Laboratories), C. Blancard (CEA, DAM, DIF,F-91297), J. Colgan (Los Alamos National Laboratory), Ph Cosse (CEA, DAM,DIF, F-91297), G. Faussurier (CEA, DAM, DIF, F-91297), Christopher Fontes(Los Alamos National Laboratory), I. Golovkin (Prism ComputationalSciences), S. Hansen (Sandia National Laboratories), C. Iglesias (LLNL), D.Kilcrease (Los Alamos National Laboratory), Joseph MacFarlane (PrismComputational Sciences), Roberto Mancini (Univeristy of Nevada), S. Nahar(Ohio State University), T. Nash (Sandia National Laboratories), ChrisOrban (Ohio State University), Marc Pinsonneault (Ohio State University),Anil Pradhan (Ohio State University), M. Sherrill (Los Alamos NationalLaboratory), B. Wilson (LLNL)

305.03 – Astrophysical Weibel instability incounterstreaming laser-produced plasmasAstrophysical shock waves play diverse roles, includingenergizing cosmic rays in the blast waves of astrophysicalexplosions, and generating primordial magnetic fieldsduring the formation of galaxies and clusters. These shocksare typically collisionless and require collectiveelectromagnetic fields to couple the upstream anddownstream plasmas. The Weibel instability has beenproposed to provide the requisite interaction mechanismfor shock formation in weakly-magnetized shocks bygenerating turbulent electric and magnetic fields in theshock front. This work presents the first laboratoryidentification of this Weibel instability betweencounterstreaming supersonic plasma flows and confirms itsbasic features, a significant step towards understandingthese shocks. In the experiments, conducted on the OMEGAEP laser facility at the University of Rochester, a pair ofplasmas plumes are generated by irradiating of a pair ofopposing parallel plastic (CH) targets. The ion-ioninteraction between the two plumes is collisionless, so asthe plumes interpenetrate, supersonic, counterstreamingion flow conditions are obtained. Electromagnetic fieldsformed in the interaction of the two plumes were probedwith an ultrafast laser-driven proton beam, and weobserved the growth of a highly striated, transverseinstability with extended filaments parallel to the flows. Theinstability is identified as an ion-driven Weibel instabilitythrough agreement with analytic theory and particle-in-cellsimulations, paving the way for further detailed laboratorystudy of this instability and its consequences for particleenergization and shock formation. [1] W. Fox, G. Fiksel, A.Bhattacharjee, P. Y. Chang, K. Germaschewski, S. X. Hu, andP. M. Nilson, “Filamentation instability of counterstreaminglaser-driven plasmas,” Phys. Rev. Lett. 111, 225002 (2013).Author(s): William Fox (University of New Hampshire), GennadyFiksel (University of Rochester), Amitava Bhattacharjee (PrincetonUniversity), Po-Yu Change (University of Rochester), Kai Germaschewski(University of New Hampshire), Suxing Hu (University of Rochester), PhilipNilson (University of Rochester)

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305.04 – Investigation of Interacting Fastand Slow Winds in Multi-ring NebulaeRing nebulae are often observed in the final stages of bluesupergiant stars. The generally accepted formationparadigm for these systems typically consists of a sparse,fast wind interacting with a previously ejected denser, slowwind. Various numerical codes have demonstrated thatsuch an interaction may explain observed ring nebulae. Wepropose a novel set of laboratory-astrophysics experimentsto investigate the interaction of these two fluids andprovide a controllable system to benchmark numericalsimulations. The experimental platform and nominal

parameters will be discussed. Support for this work wasprovided by NASA through Einstein Postdoctoral Fellowshipgrant number PF3-140111 awarded by the Chandra X-rayCenter, which is operated by the Astrophysical Observatoryfor NASA under contract NAS8-03060. This work is fundedby the NNSA-DS and SC-OFES Joint Program in High-Energy-Density Laboratory Plasmas, grant number DE-NA0001840and by the Predictive Sciences Academic Alliances Programin NNSA-ASC via grant DEFC52- 08NA28616. Work by LLNLwas performed under the auspices of U.S. DOE undercontract DE-AC52-07NA27344.Author(s): Mario Manuel (Smithsonian Astrophysical Observatory),R. Paul Drake (University of Michigan)

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306 – Education and HistoryOral Session – Gloucester, 2nd Floor – 04 Jun 2014 10:00 AM to 11:30 AMChair(s):Jay Pasachoff (Williams College)

306.01 – Higher Education Resources fromthe NASA SMD Astrophysics ForumThe NASA Astrophysics Science Education and PublicOutreach Forum (SEPOF) coordinates the work of individualNASA Science Mission Directorate (SMD) Astrophysics EPOprojects and their teams into a coherent, effective, efficient,and sustainable effort. The Astrophysics Forum assistsscientists and educators with becoming involved in SMDE/PO and makes SMD E/PO resources and expertiseaccessible to the science and education communities. Herewe describe how the Astrophysics Forum and theAstrophysics E/PO community have focused efforts tosupport and engage the higher education community onenhancing awareness of the resources available to them. Toensure Astrophysics higher education efforts are groundedin audience needs, we held informal conversations withinstructors of introductory astronomy courses, convenedsessions with higher education faculty and E/POprofessionals at conferences, and examined existingliterature and findings of the SMD Higher EducationWorking Group. To address the expressed needs, theAstrophysics Forum collaborated with the Astrophysics E/POcommunity, researchers, and Astronomy 101 instructors toplace individual science discoveries and learning resourcesinto context for higher education audiences. Among theseresources are two Resource Guides on the topics ofcosmology and exoplanets. These fields are ripe withscientific developments that college instructors have toldus they find challenging to stay current. Each guideincludes a wide variety of sources and is available throughthe ASP website: http://www.astrosociety.org/education/astronomy-resource-guides/ To complement the resourceguides, we are developing a series of slide sets to helpAstronomy 101 instructors incorporate new discoveriesfrom individual SMD Astrophysics missions in theirclassrooms. The “Astro 101 slide sets” are 5-7 slidepresentations on a new development or discovery from aNASA SMD Astrophysics mission relevant to an Astronomy101 topic. We intend for these slide sets to help Astronomy101 instructors include new, unfamiliar developments(discoveries not yet in their textbooks) into the“big-picture” context of the course.Author(s): Bonnie Meinke (STScI), Gregory Schultz (AstronomicalSociety of the Pacific), James Manning (NASA Astrophysics SEPOF), DeniseSmith (STScI), Luciana Bianchi (Johns Hopkins University), William Blair(Johns Hopkins University), Andrew Fraknoi (Foothill College)

Contributing teams: the Astrophysics E/PO community

306.02 – Leveraging Cognitive ScienceUnderpinnings to Enhance NGSS AstronomyConceptsNational-scale science education reform efforts have beenhampered by highly fragmented frameworks and standardsthat vary considerably from one state to the next. In aneffort to improve the quality of science education acrossthe nation’s K-12 schools, the 2013 Next GenerationScience Standards (NGSS) have been designed to guidestates in specifying the learning targets and performanceexpectations of all K-12 students. The NGSS is designed toreflect the 2011 Framework for K-12 Science Educationdeveloped by the National Research Council of the NationalAcademy of Sciences. As teachers, curriculum developers,and assessment experts begin to implement the NGSS inspecific geographical and socio-economic contexts, movingbeyond an examination of common student misconceptionsand reasoning difficulties to delineate the specific cognitivesources of those difficulties, and the specific interventionsthat can serve as countermeasures, should be a fruitfulnext step. While astronomy education researchers havealready documented challenges in teaching systemprocesses that operate with the space system, solarsystem, and interconnected Earth science systems, we arefar from a thorough understanding of student thinking inastronomy. Many of these ideas can be better taught-andtested-by carefully examining the underlying cognitivescience including learners’ difficulties with spatial thinkingand the prescribed astronomy and space science concepts.The NGSS may prove to be useful as a framework for nextsteps in the cognitive science within astronomy, and thiswork may benefit from deliberate collaborations betweeneducation researchers, curriculum developers, and thosewho engage in teacher professional development.Author(s): Stephanie Slater (CAPER Center for Astronomy &Physics Education Research), Timothy Slater (University of Wyoming)

306.03 – The Pulsar Quartet: Listening to aGalactic SymphonyPulsars are exotic dead stars that emit very regular radiopulses. These pulses are attributed to their regular rotation.Some pulsars are spinning fast enough that the audioequivalent waveform of their pulses fall within our hearingrange. If human ears were tuned to radio waves it wouldhave been possible to ‘hear’ these very compact stars. Weproduced the audio waveform of these pulsar signals andmapped them onto a frequency chart to find thecorresponding musical notes. We use these ‘audible'pulsars like musical instruments in a symphony orchestra toplay a full quartet. At the same time, an accompanyingvisual interface shows the realistic distribution of all pulsarsin our own Galaxy. Pulsars shine as they play each note inthe quartet with realistic brightening and subsequentdimming proportional to their rotational energies. This canserve as an educational tool at all levels to demonstratemany interesting aspects of stellar evolution and articulatean aesthetic connection of us with the cosmos. Interestedin watching the light show while the Milky Way PulsarOrchestra plays a quartet?Author(s): Bülent Kiziltan (Harvard-Smithsonian Center forAstrophysics)

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306.04 – Nova Discovery Efficiency1890-2014; Only 43%±6% of the BrightestNova Are DiscoveredGalactic nova discovery has always been the domain of thebest amateur astronomers, with the only substantialexception being the use of the Harvard plates from1890-1947. (Modern CCD surveys have not produced anysignificant nova discoveries.) From 1890-1946, novae werediscovered by gentlemen who deeply knew the stars in thesky and who checked for new stars on every clear night.This all changed when war surplus binoculars becamecommonly available, so the various organizations (e.g.,AAVSO, BAA) instructed their hunters to use binoculars toregularly search small areas of the Milky Way. In the 1970sthe hunters largely switched to blinking photographs, whilethey switched to CCD images in the 1990s, all exclusivelyin Milky Way regions. Currently, most hunters use 'go-to'scopes to look deeply only in the Milky Way, use weekly ormonthly cadences, never go outside to look up at the light-polluted skies, and do not have the stars memorized at all.This situation is good for catching many faint novae, but isinefficient for catching the more isotropic andsystematically-fast bright novae. I have made anexhaustive analysis of all known novae to isolate the effectson the relative discovery efficiency as a function of decade,the elongation from the Sun, the Moon's phase, thedeclination, the peak magnitude, and the duration of thepeak. For example, the relative efficiency for novae southof declination -33° is 0.5 before 1953, 0.2 from 1953-1990,and 0.8 after 1990. My analysis gives the overall discoveryefficiency to be 43%±6%, 30%, 22%, 12%, and 6% fornovae peaking brighter than 2, 4, 6, 8, and 10 mag. Thus,the majority of first magnitude novae are being missed. Thebright novae are lost because they are too close to the Sun,in the far south, and/or very fast. This is illustrated by thediscovery rate for Vpeak<2 novae being once every fiveyears before 1946, yet only one such nova (V1500 Cyg) hasbeen seen in the last 68 years. A critical consequence ofthis result is that the nova rate for our Milky Way hasdoubled.Author(s): Bradley Schaefer (Louisiana State Univ.)

306.05 – The first published chart of theAndromeda Nebula, 1667The Parisian astronomer Ismaél Bullialdus (1605–1694) isknown for his planetary tables (Astronomia philolaica,1645) based on a geometrical approximation to theKeplerian ellipse, and for his long correspondence with theDanzig astronomer Johannes Hevelius and with ChristiaanHuygens. Bullialdus became interested in the nascent studyof variable stars, and in 1667 published a small pamphletwith two contributions, one on Mira Ceti and the other onthe nebula in Andromeda. He found a manuscriptportraying the nebula with the date 1428, and becauseTycho Brahe never mentioned a nebula in Andromeda,Bullialdus conjectured that this object was a variable thathad disappeared in the intervening era. “We conclude thissince this conglomeration was observed neither byHipparchus nor anyone else in antiquity, nor in the previousage by Tycho, nor in the age of our forefathers like Bayer.”His publication included a handsome engraving of theimage of Andromeda and the position of the nebula, its firstprinted chart. I recently acquired a copy of this rarepamphlet, Ad astronomos monita duo, and realized that theimage matched a manuscript now in the Gotha ResearchLibrary, a 15th-century Latin version based on the work ofthe tenth-century Islamic astronomer, al-Sufi. Themanuscript does not carry the name of al-Sufi, and henceBullialdus had no real clue about its origin or its date ofcomposition. Paul Kunitzsch (The Arabs and the Stars,1989, Article XI, “The Astronomer Abu ’l-Husayn al-Sufi”)has identified a group of eight “Latin al-Sufi” manuscriptsfrom this period, scattered in European libraries, but onlythe one now in Gotha is an exact match to Bullialdus’engraving. The al-Sufi manuscript was given to the GothaLibrary in 1798 by Duke Ernst II of Saxonia-Gotha-Altenburg, who must have acquired it from Francesometime in the 18th century.Author(s): Owen Gingerich (Harvard-Smithsonian, CfA)

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306.06 – The Portrayal of the MediceanMoons in Early Astronomical Charts andBooksGalileo’s talents in perspective and chiaroscuro drawing ledto his images of the Moon being accepted as the portrayalof a truly natural physical place. The Moon was seen as aworld—real but separate from Earth. In contrast to hisresolved views of the Moon, Galileo saw the moons ofJupiter as only points of light, and thus in Sidereus Nunciusthey appear as star-symbols. Within 50 years, in Cellarius’Atlas Coelestis seu Harmonia Macrocosmica (1660), theMedicean moons continue to appear in multiple charts asstar-shaped symbols—in most cases equidistant fromJupiter. They appear in the Cellarius charts as updates tothe cosmological systems of Copernicus and Tycho Brahe,but not in the charts devoted to the Ptolemaic system. Aquarter century later, Mallet did not include the moons ofJupiter in his Copernican chart in Description de l’Universe(1683). Around 1690, in Jaillot’s Four Systems ofCosmology, the Medicean moons appear as circularsymbols in four distinct concentric orbits around Jupiter.

Additional examples appear in a later edition of Mallet((1690s), and in De Fer (1705), Dopplemayer (1720), andstill later in Buy de Mornas (1761). As objects discussed inscientific book, symbolic representations of the Mediceanmoons appear in Marius (1614), Descartes (1644), Fontana(1646) and Hevelius (1647). A pictorial survey ofantiquarian charts and books depicting the Mediceanmoons will be the focus of this presentation. As telescopesizes increased, the Galilean moons could be seen asextended objects, and thus the transition occurred fromportraying the moons as points of light to disks withphysically-meaningful details. Initially, these were done viadrawings of glimpses of the disks of the four moons duringmoments of extremely good seeing (termed “lucky images”in the pre-adaptive optics period). This era of portrayingsurface characteristics of Io, Europa, Ganymede andCallisto by hand-drawn images from naked-eyeobservations ended in the 1970s when spaceflight missionsto the outer planets returned photographic images.Author(s): Michael Mendillo (Boston University)

307 – Sebastian Heinz: Jets On All Scales: A Phenomenological View ofCollimated Outflows and Their Importance for Cosmic StructurePlenary Session – America Ballroom North/Central – 04 Jun 2014 11:40 AM to 12:30 PMChair(s):Chryssa Kouveliotou (NASA/MSFC)

307.01 – Jets on all scales: aphenomenological view of collimatedoutflows and their importance for cosmicstructureThe concept of a relativistic jet is simple: A bundled flow ofmomentum and energy, launched by an accretion flow ontoa massive compact object - most commonly a black hole.Phenomenologically, jets do indeed show a range of simpleproperties that connect them across a wide range of scales:similar radiative processes and observational signatures,similar efficiencies in converting accreted mass to outflowenergy, similar morphologies. This common, apparentsimplicity in observable properties hides the complexplasma astrophysics at work in the creation of the oftenultra-relativistic flows we observe in extragalactic jets. It

indicates that the underlying processes, if not simple, areat least similar in a wide range of objects and suggests thatwe may learn a lot about the properties of jets and thecentral engines that create them even in the absence of acomplete understanding of jet acceleration and collimation.The scientific benefit of such an approach can besignificant: For example, we now know that jets areenergetically important in the context of cosmic structureformation and galaxy evolution, and phenomenologicalscaling models can provide well calibrated models for howjets impact their environments. I will present an overview ofjet phenomenology and how an integrated view of theproblem for a wide range of black hole properties caninform models of jet creation as well as global models offeedback on interstellar and intergalactic scales.Author(s): Sebastian Heinz (Univ. Of Wisconsin, Madison)

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311 – On the Shoulders of Giants: Planets Beyond the Reach of Kepler IV: TheNear FutureMeeting-in-a-Meeting – America Ballroom North/Central – 04 Jun 2014 02:00 PM to 03:30 PM

What kind of planets lie at orbit radii of 1-2 AU - beyond the reach of Kepler? In the last two decades we haveexplored a large sample of RV-detected and transit-detected planets, discovered distant planets with microlensingand several hot young planets at large radii using direct imaging, as well as the debris disks that provide clues toformation and evolution. In these 4 sessions, we explore the near future, and how we can expect to learn muchmore about the demographics and properties of cold outer planets. WFIRST-AFTA will open up this area, with amicrolensing survey to probe the population of long-orbit planets, and coronagraphy to take images and spectraof large planets in orbits at a few AU. Session IV covers what we can expect to learn about this planet populationin the near future. In addition to TESS and JWST under development, we also discuss the contributions ofAFTA-WFIRST through microlensing and spectroscopy.

Chair(s):Thomas Greene (NASA Ames Research Center)


311.01 – Overview of WFIRST-AFTA MissionCapabilitiesWide-Field Infrared Survey Telescope (WFIRST), thetop-priority mission in the 2010 Astronomy & AstrophysicsDecadal Survey, is now planned to use an already-built2.4m telescope obtained from the National ReconnaissanceOrganization. This telescope provides image clarity similarto HST, but with an optical design and array ofnew-generation H4RG infrared detectors that enablesimaging of 100 times the area of HST in a single exposure.This wide-field IR instrument will provide galaxy surveysand supernova monitoring for dark energy studies that aresignificantly deeper than those planned by otherobservatories. A microlensing survey of the galactic bulgewill give a census of exoplanets that is at larger distance tothe Kepler sample. A coronagraph instrument will directlyimage ice and gas giant planets, and circumstellar disks.There will be significant opportunities for guest observerscience. The talk will summarize capabilities and currentstatus.Author(s): Neil Gehrels (NASA's GSFC)

311.02 – Mass Measurements for MicrolensPlanets with WFIRST/AFTAUnlike ground-based surveys, WFIRST/AFTA will be able tosystematically measure masses of the lens stars (andhence their planets) for a large number of microlensingevents. I will review the methods WFIRST/AFTA will use tomeasure masses (detection of lens light, microlensparallax, and astrometric microlensing) and present a fewexamples of how these techniques have been applied todate. These mass measurements are important forunderstanding the planet population and characterizingstructures in the planet mass function beyond the snowline. In addition, they can be used to measure the stellarmass function from black holes to brown dwarfs andunambiguously identifying free-floating planets.Author(s): Jennifer Yee (Harvard Smithsonian CfA)

311.03 – WFIRST-AFTA: What Can We Learnby Detecting Thousands of Cold Exoplanetsvia Microlensing?The WFIRST-AFTA microlensing survey will monitor a fewhundred million stars in the Galactic bulge every ~15minutes to measure the microlensing signatures ofthousands of both bound and free-floating planets withmasses ranging from super-Jupiters down to that ofGanymede. This huge sample of cold planets will perfectlycompliment the sample of warm and hot planets that havebeen found by Kepler and will be further expanded by TESSand PLATO. I will review the measurements thatWFIRST-AFTA will make for each of the planets it finds, andattempt to predict the impact that these will have on ourunderstanding of exoplanet demographics and the planetformation process.Author(s): Matthew Penny (Ohio State University)

311.04 – Capabilities of WFIRST-AFTA forcoronagraphic imaging of exoplanetsThe coronagraph on WFIRST-AFTA will be capable ofdetecting all known radial velocity planets within its rangeof angular sensitivity, and of characterizing them withphotometry and spectroscopy. The coronagraph will also becapable of detecting as-yet unknown exoplanets, from gasgiants down to super-Earths around nearby stars, andzodiacal dust disks down to the level of a few times thesolar system zodi.Author(s): Wesley Traub (Jet Propulsion Laboratory)

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311.05 – Observing Other Worlds With JWSTExoplanet science is one of the four highest level sciencethemes identified by the JWST project. And indeed, JWSToffers dramatic capabilities for characterizing exoplanetswith all four of its science instruments. The major observingmodes will be coronagraphic imaging, transit photometry,and transit spectroscopy. Both the near-IR camera, NIRCam,and the mid-IR instrument, MIRI, have coronagraphs whichwill be able to image directly young planets orbiting nearbystars. While 8-10 m ground-based telescopes equipped withExtreme AO can work at smaller inner working angles, JWSTwill offer unprecedented sensitivity at 3-20 um outside of~1” (~4 lam/D at 5 um). At these angular separations JWSTwill push the detection limit for young planets orbiting at~10-200 AU down to roughly the mass of Saturn frompresent-day limits of a few times the mass of Jupiter. Thisimaging will be carried out using a variety of narrow-,medium- and broad filters to characterize exoplanet orbitsand atmospheres. NIRCam and MIRI coronagraphs will alsomake detailed maps of bright debris disks to investigatetheir shapes and composition. All four instruments havephotometric and spectroscopic capabilities for transitobservations. NIRCam and MIRI will study primary andsecondary transits and obtain full orbital light curves in avariety of photometric filters with precision much betterthan 100 ppm. NIRCam and the Canadian instrument,NIRISS, have grism spectrometers which together span the1-5 um region at resolutions of a R~300-2,000. NIRSpechas prism and spectrometer modes with spectralresolutions ranging from R=30- 3,000 across the 1-5 umregion. MIRI has spectrometer and grism capabilitiesextending out to 30 um. These spectra and light curves willbe used to investigate atmosphere composition, surfacegravity, vertical structure, and horizontal flows. Withexoplanet research identified as one of JWST’s four highestlevel science themes, the exoplanet community should beplanning a wide variety of programs that will be strongenough to capture 25% of JWST’s observing time.Author(s): Charles Beichman (JPL)

311.06 – Exo-S: A Probe-scale Space Missionto Directly Image and SpectroscopicallyCharacterize Exoplanetary Systems Using aStarshade and Telescope System"Exo-S" is NASA's first directed community study of astarshade and telescope system for space-based discoveryand characterization of exoplanets by direct imaging. Undera cost cap of $1B, Exo-S will use a modestly sizedstarshade (also known as an "external occulter") and amodest aperture space telescope for high contrastobservations of exoplanetary systems. The Exo-S will obtainspectra of a subset of its newly discovered exoplanets aswell as already known Jupiter-mass exoplanets. Exo-S willbe capable of reaching down to the discovery of Earth-sizeplanets in the habitable zones of twenty sun-like stars, witha favorable few accessible for spectral characterization. Wepresent highlights of the science goals, the mission design,and technology milestones already reached. At the studyconclusion in 2015, NASA will evaluate the Exo-S conceptfor potential development at the end of this decade.Author(s): Sara Seager (Massachusetts Institute of Technology),Webster Cash (University of Colorado), N. Kasdin (Princeton University),William Sparks (STScI), Margaret Turnbull (Global Science Institute), MarcKuchner (NASA GSFC), Aki Roberge (NASA GSFC), Shawn Domagal-Goldman (NASA GSFC), Stuart Shaklan (NASA-JPL/Caltech), Mark Thomson(NASA-JPL/Caltech), Doug Lisman (NASA-JPL/Caltech), Suzanne Martin(NASA-JPL/Caltech), Eric Cady (NASA-JPL/Caltech), David Webb (NASA-JPL/Caltech)

311.07 – Exo-C: A probe-scale space missionto directly image and spectroscopicallycharacterize exoplanetary systems using aninternal coronagraph"Exo-C" is NASA's first community study of a modestaperture space telescope designed for high contrastobservations of exoplanetary systems. The mission will becapable of taking optical spectra of nearby exoplanets inreflected light, searching for previously undetected planets,and imaging structure in a large sample of circumstellardisks. We present the mission/payload design and highlightsteps to reduce mission cost/risk relative to previousmission concepts. At the study conclusion in 2015, NASAwill evaluate it for potential development at the end of thisdecade.Author(s): Karl Stapelfeldt (NASA Goddard Space Flight Center),Michael Brenner (Jet Propulsion Laboratory, California Institute ofTechnology), Keith Warfield (Jet Propulsion Laboratory, California Instituteof Technology), Ruslan Belikov (NASA Ames Research Center), PaulBrugarolas (Jet Propulsion Laboratory, California Institute of Technology),Geoffrey Bryden (Jet Propulsion Laboratory, California Institute ofTechnology), Kerri Cahoy (Massachusetts Institute of Technology), SupriyaChakrabarti (University of Massachusetts), Frank Dekens (Jet PropulsionLaboratory, California Institute of Technology), Robert Effinger (JetPropulsion Laboratory, California Institute of Technology), Brian Hirsch (JetPropulsion Laboratory, California Institute of Technology), Andrew Kissil (JetPropulsion Laboratory, California Institute of Technology), John Krist (JetPropulsion Laboratory, California Institute of Technology), Jared Lang (JetPropulsion Laboratory, California Institute of Technology), Mark Marley(NASA Ames Research Center), Michael McElwain (NASA Goddard SpaceFlight Center), Victoria Meadows (University of Washington), Joel Nissen(Jet Propulsion Laboratory, California Institute of Technology), Jeffrey Oseas(Jet Propulsion Laboratory, California Institute of Technology), GeneSerabyn (Jet Propulsion Laboratory, California Institute of Technology), EricSunada (Jet Propulsion Laboratory, California Institute of Technology),Wesley Traub (Jet Propulsion Laboratory, California Institute of Technology),John Trauger (Jet Propulsion Laboratory, California Institute of Technology),Stephen Unwin (Jet Propulsion Laboratory, California Institute ofTechnology)

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312 – Corona IMeeting-in-a-Meeting – America Ballroom South – 04 Jun 2014 02:00 PM to 03:30 PMChair(s):Nicholeen Viall (NASA Goddard Space Flight Center)

312.01D – The Heating of Active RegionsUsing Active Region Transient BrighteningsObserved with XRT and Hi-CActive region transient brightentings (ARTBs) are amongthe smallest and most fundamental of energetic transientevents in the corona; as such, they provide a testbed formodels of heating and active region dynamics. We havemodeled a large collection of ARTBs observed withHinode/XRT and with Hi-C as both (a) multi-stranded loopsand (b) monolithic loops which experience multiple heatingevents, to explore the energetic ramifications andcharacteristics in active region dynamics. Even for thesesmall, short-lived transients, our modeling indicates thatmultiple heating events are required for each ARTB. Wecompare the quality of model fits for two different temporalenvelopes of the heating function, and discuss whether theresults more strongly favor nanoflare or wave-absorptionheating.Author(s): Adam Kobelski (Montana State University), DavidMcKenzie (Montana State University)

312.02 – Distribution of electric currents insource regions of solar eruptionsThere has been a long-lasting debate on the question ofwhether or not electric currents in the source regions ofsolar eruptions are neutralized. That is, whether or not thedirect coronal currents connecting the photosphericpolarities in such regions are surrounded by return currentsof equal amount and opposite direction. In order to addressthis question, we consider several mechanisms of sourceregion formation (flux emergence, photosphericshearing/twisting flows, and flux cancellation) and quantifythe evolution of the electric currents, using 3D MHDsimulations. For the experiments conducted so far, we finda clear dominance of the direct currents over the returncurrents in all cases in which the models producesignificant magnetic shear along the source region'spolarity inversion line. This suggests that pre-eruptivemagnetic configurations in strongly sheared active regionsand filament channels carry substantial net currents. Wediscuss the implications of this result for the modeling ofsolar eruptions.Author(s): Tibor Torok (Predictive Science, Inc.), James Leake(George Mason University), Viacheslav Titov (Predictive Science, Inc.),Vasilis Archontis (University of St. Andrews), Zoran Mikic (PredictiveScience, Inc.), Mark Linton (U.S. Naval Research Lab), Kevin Dalmasse(Observatoire de Paris), Guillaume Aulanier (Observatoire de Paris),Bernhard Kliem (Universität Potsdam)

312.03 – Verification of Loop DiagnosticsMany different techniques have been used to characterizethe plasma in the solar corona: density-sensitive spectralline ratios are used to infer the density, the evolution ofcoronal structures in different passbands is used to inferthe temperature evolution, and the simultaneous intensitiesmeasured in multiple passbands are used to determine theemission measure. All these analysis techniques assumethat the intensity of the structures can be isolated throughbackground subtraction. In this paper, we use simulatedobservations from a 3D hydrodynamic simulation of acoronal active region to verify these diagnostics. Thedensity and temperature from the simulation are used togenerate images in several passbands and spectral lines.We identify loop structures in the simulated images andcalculate the loop background. We then determine thedensity, temperature and emission measure distribution asa function of time from the observations and compare withthe true temperature and density of the loop. We find thatthe overall characteristics of the temperature, density, andemission measure are recovered by the analysis methods,but the details of the true temperature and density are not.For instance, the emission measure curves calculated fromthe simulated observations are much broader than the trueemission measure distribution, though the averagetemperature evolution is similar. These differences are due,in part, to inadequate background subtraction, but alsoindicate a limitation of the analysis methods.Author(s): Amy Winebarger (NASA MSFC), Roberto Lionello (PredictiveScience, Inc), Yung Mok (University of California), Jon Linker (PredictiveScience, Inc), Zoran Mikic (Predictive Science, Inc)

312.04 – Evidence for Impulsive CoronalHeating from EUNIS 2013Pervasive, faint Fe XIX 592 Å line emission was observed inactive regions by the Extreme Ultraviolet Normal IncidenceSpectrograph (EUNIS) sounding rocket instrument on 23April 2013. The broad spectral coverage (303-370 Å,527-635 Å) and unprecedented dynamic range of the EUNISobservations includes emission lines of ionization stagesfrom He I to Fe XX, and thus a wide temperature range of0.03 to 10 MK. Comparison of observed line intensities withcalculations demonstrates that the Fe XIX emission, formedat temperatures around 8 MK, is evidence of the faint hotemission predicted by impulsive heating models of thesolar corona (such as nanoflares).Author(s): Adrian Daw (NASA Goddard Space Flight Center), JeffreyBrosius (NASA Goddard Space Flight Center), Douglas Rabin (NASAGoddard Space Flight Center), Enrico Landi (University of Michigan), JamesKlimchuk (NASA Goddard Space Flight Center)

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312.05 – The Hydrodynamics of HighTemperature Plasma: Reproducing theProperties of High Temperature Emission inSolar Active RegionsThe launch of Hinode and SDO have revolutionized ourability to measure the plasma properties of the solarcorona. Many studies have documented both thetemperature structure of the corona as well as its temporalvariability. Of particular interest is the behavior of hightemperature loops that are typically found in the core of anactive region. Temperature distributions in these regionsare often sharply peaked near 4 MK but rapidly evolvingloops are also observed. In this talk we will present resultsfrom our effort to perform hydrodynamic simulations of 15solar active regions that cover a wide range of solarconditions and to reconcile these simulations withobservations. In this work we have coupled non-linear forcefree extrapolations with solutions to the hydrodynamic loopequations approximated by EBTEL. Using relatively simpleheating scenarios we are able to reproduce three importantproperties of the observations: the dependance of theobserved intensity on magnetic flux, the sharply peakedemission measure distributions for large regions, and thegeneral frequency distribution of the observed events. Ourcurrent simulations, however, suggest much stronger 1MKemission near the neutral line than is observed, indicatingthe heating of small loops is not well understood. We alsodo not properly reproduce the relative distribution of largeand small events in these active regions.Author(s): Ignacio Ugarte-Urra (George Mason University), HarryWarren (Naval Research Laboratory)

312.06 – Dynamic moss observed with Hi-CThe High-resolution Coronal Imager (Hi-C), flown on 11 July2012, has revealed an unprecedented level of detail andsubstructure within the solar corona. Hi-C imaged a largeactive region (AR11520) with 0.2-0.3’’ spatial resolutionand 5.5s cadence over a 5 minute period. An additionaldataset with a smaller FOV, the same resolution, but with ahigher temporal cadence (1s) was also taken during therocket flight. This dataset was centered on a large patch of‘moss’ emission that initially seemed to show very littlevariability. Image processing revealed this region to bemuch more dynamic than first thought with numerousbright and dark features observed to appear, move anddisappear over the 5 minute observation. Moss is thoughtto be emission from the upper transition region componentof hot loops so studying its dynamics and the relationbetween the bright/dark features and underlying magneticfeatures is important to tie the interaction of the differentatmospheric layers together. Hi-C allows us to study thecoronal emission of the moss at the smallest scales whiledata from SDO/AIA and HMI is used to give information onthese structures at different heights/temperatures. Usingthe high temporal and spatial resolution of Hi-C theobserved moss features were tracked and the distributionof displacements, speeds, and sizes were measured. Thisallows us to comment on both the physical processesoccurring within the dynamic moss and the scales at whichthese changes are occurring.Author(s): Caroline Alexander (NASA/MSFC), Amy Winebarger(NASA/MSFC), Richard Morton (Northumbria University), Sabrina Savage(NASA/MSFC)

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313 – Chromosphere and Transition Region (IRIS)Meeting-in-a-Meeting – Staffordshire – 04 Jun 2014 02:00 PM to 03:30 PMChair(s):Bart De Pontieu (Lockheed Martin Solar and Astrophysics Lab)

313.01 – Coordinated IRIS science using theHeliophysics Event KnowledgebaseWe have recently enhanced the capabilities of theHeliophysics Event Knowledgebase (HEK) to support thecomplex datasets being produced by the Interface RegionImaging Spectrograph (IRIS). This includes tools toincorporate observations from the Solar DynamicsObservatory and ground-based facilities to generatecomposite data products. We will discuss the system and itsrecent evolution and demonstrate its ability to supportcoordinated science investigations.Author(s): Neal Hurlburt (Lockheed Martin Corp.), Sam Freeland(Lockheed Martin Corp.), Ryan Timmons (Lockheed Martin Corp.), Bart DePontieu (Lockheed Martin Corp.)

313.02 – IRIS Observations of Twist in theLow Solar AtmosphereThe Interface Region Imaging Spectrograph (IRIS) smallexplorer was launched in June 2013. IRIS’s high-resolution(0.33 arcsec), high-cadence (2s) images and spectra reveala solar chromosphere and transition region that is riddledwith twist. This is evidenced by the presence of ubiquitoustorsional motions on very small (subarcsec) spatial scales.These motions occur in active regions, quiet Sun andcoronal holes on a variety of structures such as spicules atthe limb, rapid-blue/red-shifted events (RBEs and RREs) aswell as low-lying loops. We use IRIS data and observationsfrom the Swedish Solar Telescope (SST) in La Palma, Spainto describe these motions quantitatively, study theirpropagation, and illustrate how such strong twistingmotions are often associated with significant and rapidheating to at least transition region temperatures.Author(s): Bart De Pontieu (University of Oslo), Luc Rouppe van derVoort (University of Oslo), Tiago M.D. Pereira (University of Oslo), HaakonSkogsrud (University of Oslo), Scott McIntosh (High Altitude Observatory),Mats Carlsson (University of Oslo), Viggo Hansteen (University of Oslo)

Contributing teams: IRIS team

313.03 – IRIS Observations of Coronal Rainand Prominences: Return Flows of theChromosphere-Corona Mass CycleIt has recently been recognized that a mass cycle (e.g.,Berger et al. 2011; McIntosh et al. 2012) between the hot,tenuous solar corona and the cool, dense chromosphereunderneath it plays an important role in the mass budgetand dynamic evolution of the solar atmosphere. Althoughthe corona ultimately loses mass through the solar windand coronal mass ejections, a fraction of its mass returns tothe chromosphere in coronal rain, downflows ofprominences, and other as-yet unidentified processes. Wepresent here analysis of joint observations of IRIS, SDO/AIA,and Hinode/SOT of such phenomena. By utilizing the widetemperature coverage (logT: 4 - 7) provided by theseinstruments combined, we track the coronal coolingsequence (e.g., Schrijver 2001; Liu et al. 2012; Berger et al.2012) leading to the formation of such material attransition region or chromospheric temperatures (logT: 4 -5) in the million-degree corona. We compare the coolingtimes with those expected from the radiative coolinginstability. We also measure the kinematics and densities ofsuch downflows and infer their mass fluxes, which arecompared to the upward mass fluxes into the corona, e.g.,those associated with spicules and flux emergence. Specialattention is paid to coronal rain formed near cusp-shapedportions of coronal loops, funnel-shaped prominences atdips of coronal loops, and their respective magneticenvironments. With the information about where and whensuch catastrophic cooling events take place, we discuss theimplications for the enigmatic coronal heating mechanisms(e.g., Antolin et al. 2010).Author(s): Wei Liu (Lockheed Martin Solar and AstrophysicsLaboratory), Thomas Berger (National Solar Observatory), Patrick Antolin(National Astronomical Observatory of Japan), Karel Schrijver (LockheedMartin Solar and Astrophysics Laboratory)

313.04 – Exploring the Components of IRISSpectra: More Shift, Twist, and Sway ThanShake, Rattle, and RollThe beautifully rich spectra of the IRIS spacecraft offer anunparalleled avenue to explore the mass and energytransport processes which sustain the Sun's outeratmosphere. In this presentation we will look in detail at thevarious components of the spectrographic data and placethem in context with Slit-Jaw imaging and EUV imagingfrom SDO/AIA. We will show that the line profiles displaymany intriguing features including the clear signatures ofstrong line-of-sight flows (in all magnetized regions) thatare almost always accompanied by transverse and torsionalmotions at the finest resolvable scales. We will demonstratethat many interesting relationships develop when studyingthe spectra statistically. These relationships indicate IRIS'sability to spectrally and temporally resolve the energeticprocesses affecting the outer solar atmosphere.Author(s): Scott McIntosh (National Center for AtmosphericResearch), Bart De Pontieu (LMSAL), Hardi Peter (MPS - Gottingen)

Contributing teams: The IRIS Team

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313.05 – Diagnostics of coronal heating andmechanisms of energy transport from IRISand AIA observations of active region mossThe variability of emission of the "moss", i.e., the uppertransition region (TR) layer of high pressure loops in activeregions provides stringent constraints on the characteristicsof heating events. The Interface Region ImagingSpectrograph (IRIS), launched in June 2013, providesimaging and spectral observations at high spatial (0.166arcsec/pix), and temporal (down to ~1s) resolution at FUVand NUV wavelengths, and together with the high spatialand temporal resolution observations of SDO/AIA, canprovide important insights into the coronal heatingmechanisms. We present here an analysis of the temporalvariability properties of moss regions at the footpoints ofhot active region core loops undergoing heating, asobserved by IRIS and AIA, covering emission from thecorona to the transition region and the chromosphere. Wemodel the observations using dynamic loop models (thePalermo-Harvard code, and RADYN, which also includes theeffects of non-thermal particles) and discuss theimplications on energy transport mechanisms (thermalconduction vs beams of non-thermal particles).Author(s): Paola Testa (Smithsonian Astrophysical Observatory),Bart De Pontieu (Lockheed Martin Solar and Astrophysics Laboratory), JoelAllred (NASA GSFC), Mats Carlsson (University of Oslo), Fabio Reale (INAF/University of Palermo), Adrian Daw (NASA GSFC), Viggo Hansteen(University of Oslo)

Contributing teams: IRIS Team

313.06 – IRIS observations of the transitionregion above sunspots: oscillations andmoving penumbral dotsNASA's IRIS mission is providing high-cadence andhigh-resolution observations of the solar transition regionand chromosphere. We present results from IRISobservation of the transition region above sunspots. Themajor findings can be summarized as following: (1) The C IIand Mg II line profiles are almost Gaussian in the sunspotumbra and clearly exhibit a deep reversal at the line centerin the plage region, suggesting a greatly reduced opacity inthe sunspot atmosphere. (2) Strongly nonlinear sunspotoscillations can be clearly identified in not only the slit jawimages of 2796Å, 1400Å and 1330Å, but also in spectra ofthe bright Mg II, C II and Si IV lines. The Si iv oscillation lagsthose of C ii and Mg ii by 6 and 25 seconds, respectively.The temporal evolution of the line core is dominated by thefollowing behavior: a rapid excursion to the blue side,accompanied by an intensity increase, followed by a lineardecrease of the velocity to the red side. The maximumintensity slightly lags the maximum blue shift in Si iv ,whereas the intensity enhancement slightly precedes themaximum blue shift in Mg ii . We find a positive correlationbetween the maximum velocity and deceleration. Theseresults are consistent with numerical simulations of upwardpropagating magneto-acoustic shock waves. We alsodemonstrate that the strongly nonlinear line widthoscillation, reported both previously and here, is spurious.(3) Many small-scale bright dots are present in thepenumbral filaments and light bridges in SJI 1330Å and1400Å images obtained in high-cadence observations. Theyare usually smaller than 1" and often just a couple of pixelswide. Some bright dots show apparent movement with aspeed of 20-60 km/s(either outward or inward). The lifetimeof these penumbral dots is mostly less than 1 min. Themost obvious feature of the Si IV profiles in the bright dotsis the enhanced line width. Besides that, the profile looksnormal and no obvious fast flows are detected. The brightdots in the light bridges even show oscillation patterns. It'snot clear whether these oscillations are triggered by theumbral oscillations or not.Author(s): Hui Tian (Harvard-Smithsonian Center forAstrophysics), Ed DeLuca (Harvard-Smithsonian Center for Astrophysics),Mark Weber (Harvard-Smithsonian Center for Astrophysics), Sean McKillop(Harvard-Smithsonian Center for Astrophysics), Kathy Reeves (Harvard-Smithsonian Center for Astrophysics), Lucia Kleint (Lockheed Martin Solarand Astrophysics Laboratory), Juan Martinez-Sykora (Lockheed MartinSolar and Astrophysics Laboratory), Bart De Pontieu (Lockheed MartinSolar and Astrophysics Laboratory), Mats Carlsson (University of Oslo)

Contributing teams: the IRIS team

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314 – Star Clusters, Binaries, Multiples, and Planetary CompanionsOral Session – St. George AB – 04 Jun 2014 02:00 PM to 03:30 PMChair(s):Edward Guinan (Villanova Univ.)

314.01 – Introducing A.S.A.D: Analyzer ofintegrated Spectra for Age DeterminationA.S.A.D (Analyzer of integrated Spectra for AgeDetermination) is a new program that can automaticallydetermine the age and reddening of stellar clusters fromtheir optical integrated spectra. We will show the results weobtained with A.S.A.D for 20 LMC clusters, and presentfurther applications for which A.S.A.D can be used whenstudying distant unresolved stellar clusters.Author(s): Randa Asa'd (American University of Sharjah), MargaretHanson (University of Cincinnati)

314.02 – The Black Hole X-ray BinaryPopulation of M51 as seen by ChandraWe present an analysis of the black hole X-ray binarypopulation of the interacting galaxy system M51 from newand archival observations by the Chandra X-rayObservatory with total exposure time of nearly 1 Ms. Thisdataset allows us to probe spectral and temporal variabilityof the X-ray source population on timescales ranging fromtens of seconds to years. We examine both theultraluminous X-ray source (ULX) population, which likelyconsists of black hole binaries based solely on luminosity,and the less luminous binaries that show evidence forharboring black holes. We further examine theenvironments of these sources within the host galaxy usingnew and archival Hubble Space Telescope observations todetermine the probable mass donor stars in the system. Wealso present initial results from an effort to study theinteraction of the luminous X-ray binaries with theinterstellar medium of M51. This sample includes all of thehistorical ULXs as well as a new transient ULX which is aprobable black hole low mass X-ray binary.Author(s): Roy Kilgard (Wesleyan Univ.), Trevor Dorn-Wallenstein(Wesleyan Univ.), K. Kuntz (Johns Hopkins University), Tyler Desjardins(University of Western Ontario)

314.03 – The Cepheid in the eclipsing binarysystem OGLE-LMC-CEP1812 is a stellarmergerClassical Cepheids and eclipsing binary systems arepowerful probes for measuring stellar fundamentalparameters and constraining stellar astrophysics. ACepheid in an eclipsing binary system is even morepowerful, constraining stellar physics, the distance scaleand the Cepheid mass discrepancy. However, thesesystems are rare, only three have been discovered. One ofthese, OGLE-LMC-CEP1812, presents a new mystery: wherethe Cepheid component appears to be younger than its redgiant companion. In this work, we present stellar evolutionmodels and show that the Cepheid is actually product of astellar merger during main sequence evolution that causesthe Cepheid to be a rejuvenated star. This result raises newquestions into the evolution of Cepheids and theirconnections to smaller-mass anomalous Cepheids.Author(s): Hilding Neilson (East Tennessee State University),Richard Ignace (East Tennessee State University)

314.04 – Transit Timing Observations of aHierarchical Triple M Dwarf SystemI will report observations of an eclipsing binary star systemin the Kepler field. Transit timing variations in the Keplerdata suggest this system may have a third, stellar-masscompanion. By obtaining several stellar spectra, we wereable to confirm the triple-star hypothesis. Transit timingobservations allow us to fully characterize the system, withanalytic approximations to the equations of motionproviding results consistent with direct 3-body numericalintegration. I will detail the system architecture, includingthe physical parameters of each object, and discuss we canlearn about the physics of M dwarfs from studying thissystem in detail.Author(s): Benjamin Montet (Harvard University), Jonathan Swift(California Institute of Technology), John Johnson (Harvard University)

314.05 – Multiplicity of Planets Among theKepler M DwarfsThe Kepler data set has furnished more than 130exoplanetary candidates orbiting M dwarf hosts, nearly halfof which reside in multiply transiting systems. I investigatethe proposition of self-similarity in this sample, first positedby Swift et al. (2013) for the analysis of the five-planetsystem Kepler-32. If we compare the predictions of a singlemode of planet multiplicity and coplanarity to the Keplersample, we find that the population of systems with twoplanets or more is well-replicated. However, the number ofsingly-transiting systems remains too high to be consistentwith this proposition, even accounting for a higher falsepositive rate among systems exhibiting only one periodictransit. I investigate astrophysical explanations for thisfeature of Kepler's multiple planet population orbiting smallstars, and explore whether the data set supports twodistinct modes of planet formation around M dwarfs. Idiscuss the relative unlikelihood of selection bias orunusually high false positive rates as an explanation, incontrast.Author(s): Sarah Ballard (NASA Carl Sagan Fellow)

314.06 – The Pan-STARRS-1 Outer SolarSystem Key Project: A Status ReportThe Pan-STARRS-1 (PS1) survey is capable of detectingslow-moving objects in the outer solar system. Amongthese are Trojans, Centaurs, long-period comets, short-period comets, and trans-neptunian objects brighter thanmagnitude R~22. We have developed a software pipeline tosearch for these objects. I will present a status report forthis pipeline, as well highlights from the PS1 Outer SolarSystem Key Project.Author(s): Matthew Holman (Harvard-Smithsonian, CfA)

Contributing teams: Pan-STARRS-1 Outer Solar Systemteam

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315 – Bridging Laboratory & Astrophysics: Nuclear and ParticlesMeeting-in-a-Meeting – St. George CD – 04 Jun 2014 02:00 PM to 03:30 PM

Laboratory astrophysics is the Rosetta Stone that enables astronomers to understand and interpret the cosmos.This session will focus on the interplay between astrophysics with theoretical and experimental studies into theunderlying nuclear processes, which drive our Universe.

Chair(s):Farid Salama (NASA Ames Research Center)

315.01 – Nuclear Astrophysics in theLaboratory and In the UniverseNuclear processes drive stellar evolution and so nuclearphysics, stellar models and observations together allow usto describe the inner workings of stars and their life stories.This information on nuclear reaction rates and nuclearproperties are critical ingredients in addressing mostquestions in astrophysics and often the nuclear database isincomplete or lacking the needed precision. Directmeasurements of astrophysically interesting reactions arenecessary and the experimental focus is on improving bothsensitivity and precision. In this talk, I will review recentresults and approaches taken at the Laboratory forExperimental Nuclear Astrophysics (LENA,http://research.physics.unc.edu/project/nuclearastro/Welcome.html). [Supported in part by the U.S. Departmentof Energy and by the National Science Foundation.]Author(s): Arthur Champagne (Triangle Universities NuclearLaboratory)

315.02 – High Energy Density Plasmas(HEDP) for studies of basic nuclear sciencerelevant to Stellar and Big BangNucleosynthesisThermonuclear reaction rates and nuclear processes havebeen explored traditionally by means of conventionalaccelerator experiments, which are difficult to execute atconditions relevant to stellar nucleosynthesis. Thus, nuclearreactions at stellar energies are often studied throughextrapolations from higher-energy data or inlow-background underground experiments. Even whenmeasurements are possible using accelerators at relevantenergies, thermonuclear reaction rates in stars areinherently different from those in accelerator experiments.The fusing nuclei are surrounded by bound electrons inaccelerator experiments, whereas electrons occupy mainlycontinuum states in a stellar environment. Nuclearastrophysics research will therefore benefit from anenlarged toolkit for studies of nuclear reactions. In thispresentation, we report on the first use of High EnergyDensity Plasmas for studies of nuclear reactions relevant tobasic nuclear science, stellar and Big Bang nucleosynthesis.These experiments were carried out at the OMEGA laserfacility at University of Rochester and the National IgnitionFacility (NIF) at Lawrence Livermore National Laboratory, inwhich spherical capsules were irradiated with powerfullasers to compress and heat the fuel to high enoughtemperatures and densities for nuclear reactions to occur.Four experiments will be highlighted in this presentation. Inthe first experiment, the differential cross section for theelastic neutron-triton (n-T) scattering at 14.1 MeV wasmeasured with significantly higher accuracy than achievedin accelerator experiments. In the second experiment, theT(t,2n)4He reaction, a mirror reaction to the3He(3He,2p)4He reaction that plays an important role inthe proton-proton chain that transforms hydrogen intoordinary 4He in stars like our Sun, was studied at energiesin the range 15-40 keV. In the third experiment, the3He+3He solar fusion reaction was studied directly, and inthe fourth experiment, we probed the T+3He reaction,possibly relevant to Big Bang nucleosynthesis.Author(s): Johan Frenje (Massachusetts Institute of Technology)

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316 – Education and Public OutreachOral Session – Gloucester, 2nd Floor – 04 Jun 2014 02:00 PM to 03:30 PMChair(s):Dawn Gelino (Caltech)

316.01 – NASA SMD Science Education andPublic Outreach Forums: A Five-YearRetrospectiveNASA’s Science Mission Directorate (SMD) created fourcompetitively awarded Science Education and PublicOutreach Forums (Astrophysics, Heliophysics, PlanetaryScience, Earth Science) in 2009. The objective is toenhance the overall coherence of SMD education and publicoutreach (E/PO), leading to more effective, efficient, andsustainable use of SMD science discoveries and learningexperiences. We summarize progress and next stepstowards achieving this goal with examples drawn fromAstrophysics and cross-Forum efforts. Over the past fiveyears, the Forums have enabled leaders of individual SMDmission and grant-funded E/PO programs to work togetherto place individual science discoveries and learningresources into context for audiences, conveying the bigpicture of scientific discovery based on audience needs.Forum-organized collaborations and partnerships extendthe impact of individual programs to new audiences andprovide resources and opportunities for educators toengage their audiences in NASA science. Similarly, Forumresources support scientists and faculty in utilizing SMDE/PO resources. Through Forum activities, mission E/POteams and grantees have worked together to definecommon goals and provide unified professionaldevelopment for educators (NASA’s MultiwavelengthUniverse); build partnerships with libraries to engageunderserved/underrepresented audiences (NASAScience4Girls and Their Families); strengthen use of bestpractices; provide thematic, audience-based entry points toSMD learning experiences; support scientists inparticipating in E/PO; and, convey the impact of the SMDE/PO program. The Forums have created a single onlinedigital library (NASA Wavelength,http://nasawavelength.org) that hosts all peer-reviewedSMD-funded education materials and worked with the SMDE/PO community to compile E/PO program metrics(http://nasamissionepometrics.org/). External evaluationshows the Forums are meeting their objectives. Specificexamples of Forum-organized resources for use byscientists, faculty, and informal educators are discussed inrelated presentations (Meinke et al.; Manning et al.).Author(s): Denise Smith (STScI), Laura Peticolas (UC-Berkeley),Theresa Schwerin (IGES), Stephanie Shipp (LPI)

Contributing teams: Astrophysics Forum Team,Astrophysics EPO Community

316.02 – The Universe Discovery Guides: ACollaborative Approach to Educating withNASA ScienceFor the 2009 International Year of Astronomy, thethen-existing NASA Origins Forum collaborated with theAstronomical Society of the Pacific (ASP) to create a seriesof monthly “Discovery Guides” for informal educator andamateur astronomer use in educating the public aboutfeatured sky objects and associated NASA science themes.Today’s NASA Astrophysics Science Education and PublicOutreach Forum (SEPOF), one of a new generation offorums coordinating the work of NASA Science MissionDirectorate (SMD) EPO efforts—in collaboration with theASP and NASA SMD missions and programs--has adaptedthe Discovery Guides into “evergreen” educationalresources suitable for a variety of audiences. The Guidesfocus on “deep sky” objects and astrophysics themes (starsand stellar evolution, galaxies and the universe, andexoplanets), showcasing EPO resources from more than 30NASA astrophysics missions and programs in a coordinatedand cohesive “big picture” approach across theelectromagnetic spectrum, grounded in best practices tobest serve the needs of the target audiences. Each monthlyguide features a theme and a representative objectwell-placed for viewing, with an accompanying interpretivestory, finding charts, strategies for conveying the topics,and complementary supporting NASA-approved educationactivities and background information from a spectrum ofNASA missions and programs. The Universe DiscoveryGuides are downloadable from the NASA Night Sky Networkweb site at nightsky.jpl.nasa.gov. The presenter will sharethe Forum-led Collaborative’s experience in developing theguides, how they place individual science discoveries andlearning resources into context for audiences, and how theGuides can be readily used in scientist public outreachefforts, in college and university introductory astronomyclasses, and in other engagements between scientists,students and the public.Author(s): Jim Manning (NASA Astrophysics SEPOF), BrandonLawton (STScI), Marni Berendsen (Astronomical Society of the Pacific),Suzanne Gurton (Astronomical Society of the Pacific), Denise Smith(STScI), The NASA SMD Astrophysics E/PO Community (NASA EPOMissions/Programs)

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316.03 – Sustaining NASA’S AstrophysicsEducation And Public Outreach ProjectsSustaining NASA’s Education and Public Outreach (E/PO)projects has been a critical element of the Science MissionDirectorate. Astrophysics E/PO programs have built robustpartnerships and publicly accessible repositories of theirproducts, which should enable them to form the bases ofnew initiatives. The recently released digital library,NASAWavelength, has a wealth of information whicheducators can use to design their own lessons, andstudents can use as a learning tool. Partnerships withlibraries, science museums and amateur astronomers hasled to targeted programs such as Astro4Girls and Night SkyNetwork. Teachers trained as Educator Ambassadors spreadthe knowledge gained through participating in NASAprograms to other educators and students. These and otherprojects will be presented in this paper as examples of self-sustaining activities, which have a multiplier effect withhigh impact. While conveying the excitement of scientificdiscoveries from NASAs Astrophysics missions, theseprojects provide a powerful means of engaging studentstowards science and technology careers.Author(s): Hashima Hasan (NASA Headquarters), Denise Smith(Space Telescope Science Institute)

316.04 – HERE, THERE, AND EVERYWHEREPublic Science Through AnalogyHere, There, and Everywhere (HTE) is a program thatconsists of a series of exhibitions, posters, and supportinghands-on activities that utilize analogies in the teaching ofscience, engineering, and technology to provide multi-generational and family-friendly content in English andSpanish to small community centers, libraries, under-resourced small science centers. The purpose of theprogram is to connect crosscutting science content (inEarth, atmospheric and planetary sciences andastrophysics) with everyday phenomena. By using differentmodes of content delivery, from physical exhibits andhandouts,to interpretive stations, facilitated activities foreducators, and online resources, HTE helps to demonstratethe universality of physical laws and the connectionbetween our everyday world and the universe as a whole tomembers of the public who may not identify strongly withscience. HTE is part of a series of public science projectscreated and developed by the Education and PublicOutreach group at the Chandra X-ray Center. The authorsdiscuss how HTE fits into the lineage of public scienceoutreach that aims to engage the greater public innon-traditional venues for science learning andappreciation, as well as what might be learned about theparticipants of such projects.Author(s): Kimberly Arcand (Smithsonian AstrophysicalObservatory)

Contributing teams: Megan Watzke, Kathleen Lestition,Susan Sunbury

316.05 – Astronomy in the InternationalYear of Light 2015In December 2013 the United Nations General Assemblyproclaimed 2015 as the International Year of Light andLight-based Technologies (IYL 2015), recognizing “theimportance of raising global awareness of how light-basedtechnologies promote sustainable development and providesolutions to global challenges in energy, education,agriculture, and health.” John Dudley, president of theEuropean Physical Society and chair of the IYL 2015Steering Committee, explains: “An International Year ofLight is a tremendous opportunity to ensure thatpolicymakers are made aware of the problem-solvingpotential of light technology. Photonics providescost-effective solutions to challenges in so many differentareas: energy, sustainable development, climate change,health, communications, and agriculture. For example,innovative lighting solutions reduce energy consumptionand environmental impact, while minimizing light pollutionso that we can all appreciate the beauty of the universe ina dark sky.” IYL 2015 is bringing together many differentstakeholders, including scientific societies and unions,educational and research institutions, technology platforms,non-profit organizations, and private-sector partners topromote and celebrate the significance of light and itsapplications during 2015. The AAS and the InternationalAstronomical Union (IAU), which were heavily involved inthe International Year of Astronomy in 2009, will play a rolein IYL 2015 — especially since the AAS will host the 29thGeneral Assembly of the IAU in August 2015. OtherUS-based organizations, such as NOAO, are organizingefforts jointly with IAU and AAS members to form acornerstone. Discussion for this presentation will center onthe IYL cornerstone project in astronomy, dark-skiesawareness, and optics and the related projects and eventsbeing formed, as well as the regional, national, andinternational committees and contact points beingestablished to ensure that all nations of the world canparticipate. Note: This abstract is adapted, in part, frompress releases by the European Physical Society and theAAS.Author(s): Constance Walker (IAU Commission 50), Stephen Pompea(NOAO), Richard Green (IAU Commission 50), Richard Fienberg (AAS),Patrick Seitzer (AAS)

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317 – Neal Evans: Star Formation in the Gould Belt: Star Formation Rates,Evolutionary Timescales, and Implications for Star Formation TheoriesPlenary Session – America Ballroom North/Central – 04 Jun 2014 03:40 PM to 04:30 PMChair(s):Edward Churchwell (Univ. of Wisconsin)

317.01 – Star Formation in the Gould Belt:Star Formation Rates, EvolutionaryTimescales, and Implications for StarFormation TheoriesResults from the c2d and Gould Belt Spitzer Legacy andHerschel Key Programs provide the most complete andaccurate information on star formation in nearby molecularclouds. Complementary and follow-up studies add crucialinformation on the nature of star forming gas and theevolution of matter as it moves from core to disk to planets.

The star formation rates and gas properties provide tests ofstar formation laws used by extragalactic researchers andof theories of large scale star formation. The durations inthe stages of star formation (envelope infall, exposed starand disk, etc.) have been refined. The data are consistentwith models in which accretion onto the forming star isepisodic, with possible consequences for the initialconditions in planet-forming disks. The evolution of thesedisks, including dust settling, volatile evolution, andgap-clearing, has been clarified.Author(s): Neal Evans (University of Texas at Austin)

400 – Newton Lacy Pierce Prize Lecture, Nadia Zakamska: Quasars and TheirEffect on Galaxy FormationPlenary Session – America Ballroom North/Central – 05 Jun 2014 08:30 AM to 09:20 AMChair(s):David Helfand (Quest University Canada)

400.01 – Quasars and their effect on galaxyformationAt the center of almost every massive galaxy is asupermassive black hole. This realization and theacceptance of the widespread existence of black holeshave been major themes in extragalactic astronomy inrecent decades. Far from being mere passive sources ofgravity, supermassive black holes may have vitallyinfluenced the formation of their host galaxies, most likely

during the active "quasar" phase of black hole growth. Inthis talk, I will outline the historic observations that haveled to the current understanding of quasars, including ourwork on obscured quasars that has helped reveal theirubiquitousness. Furthermore, I will describe how newobservations of quasar winds are beginning to tie togetherthe theoretical threads linking quasar and galaxy formationand providing direct insight into the details of thelong-sought phenomenon of quasar feedback.Author(s): Nadia Zakamska (Johns Hopkins University)

– LAD Posters ThursdayPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 06:00 PM

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413 – LAD Late PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

413.01 – Development of a supersonic,single-mode, shockwave-driven Kelvin-Helmholtz instability experimentHydrodynamic instabilities are ubiquitous in high-energy-density systems, including core collapse supernovae andprotoplanetary disks. The Kelvin-Helmholtz instabilityevolves from shear flow at an interface and results inmixing between the two layers. This poster will cover tworecent experiments studying the evolution of asingle-mode, supersonic case of the Kelvin-Helmholtzinstability with well-characterized initial conditions.Classically, the growth rate of the Kelvin-Helmholtzinstability increases as the relative shear velocity of thesystem increases. When the relative velocity becomes verylarge, compressibility effects begin to inhibit Kelvin-Helmholtz growth. In our experiment we create a steady,high Mach number flow by driving our instability with ashockwave generated by a 20 to 30 ns laser pulse. We seedperturbation growth with a precisely machined,well-characterized, single-mode sinusoidal interface. Thesystem is diagnosed using Spherical Crystal Imaging, aform of x-ray radiography. This work is funded by the U.S.Department of Energy, through the NNSA-DS and SC-OFESJoint Program in High-Energy-Density Laboratory Plasmas,grant number DE-NA0001840, the National Laser UserFacility Program, grant number DE-NA0000850, and theLaboratory for Laser Energetics, University of Rochester bythe NNSA/OICF under Cooperative Agreement No.DE-FC52-08NA28302.Author(s): Wesley Wan (University of Michigan), Guy Malamud(Nuclear Research Center), Carlos Di Stefano (University of Michigan), MattTrantham (University of Michigan), Sallee Klein (University of Michigan),Assaf Shimony (Nuclear Research Center), Dov Shvarts (Nuclear ResearchCenter), Carolyn Kuranz (University of Michigan), R. Paul Drake (Universityof Michigan)

413.02 – Modeling the Infrared Emission ofHigh-Latitude Molecular Cirrus CloudsThe exact amount and nature of interstellar matter at highGalactic latitudes is a subject of ongoing scrutiny. The IRASobservations at 60 and 100 micrometer first revealed theprevalence of large-scale, extended filamentary emission(known as ``infrared cirrus'', see Low et al. 1984) at highGalactic latitudes. The presence of significant quantities ofCO gas at high Galactic latitudes (|b|>25 degree) was firstreported by Blitz et al. (1984) and Magnani et al. (1985).These high latitude molecular clouds can be identified withthe cores of the IRAS infrared cirrus (Weiland et al. 1986).Little is known about the dust properties of these highlatitude molecular cirrus clouds. We model the infraredemission of nine representative clouds (Verter et al. 2000)for which the visual extinction (A_V) was known from starcounts (Magnani & de Vries 1986). All the selected clouds,with A_V <1 mag, are "translucent" to the interstellarradiation. They represent a class of objects intermediatebetween the properties of diffuse clouds and darkmolecular clouds (van Dishoeck & Black 1988). They exhibitnotable cloud-to-cloud variations in the mid-infrared, withthe ratio of the IRAS 12 micrometer intensity to the IRAS 25micrometer intensity varying by up to one order ofmagnitude. The silicate-graphite-PAH model successfullyreproduces the infrared emission of all the selected cloudsobserved by IRAS. We find that all clouds are rich in PAHs astraced by the IRAS 12 micrometer data. They are heated bythe local interstellar radiation field, but with the radiationintensity reduced by a factor of about 2 to 3.Author(s): Ajay Mishra (University of MIssouri-Columbia), Aigen Li(University of MIssouri-Columbia)

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413.03 – Irradiation of oxygen and waterices at by 4 keV singly and doubly chargedions; sputtering and molecular synthesisThe icy surfaces of dust grains in the Interstellar Mediumand those of comets, satellites and Kuiper Belt Objects arecontinuously exposed to photon and charged particleirradiation. These energetic particles may sputter andinduce chemical changes in the ices and the underlyingsurfaces. In the present work 258 nm thick O2 and H2Oices were deposited at 10 K with the thickness measured bya laser interferometer method. A simple model fit to thereflected laser intensity as measured by a photodiodedetector enabled the refractive index of the ices to bedetermined. The ices were then irradiated with varioussingly and doubly charged ions such as He+, 13C+, N+, O+, Ar+, 13C2+, N2+ and O2+ at 4 keV. The decrease in icethickness as a function of ion dose was monitored by alaser interferometer and the model used to determine thesputtering yield as shown in Figure 1. In the case of O2 icethe sputtering yields increased with increasing ion mass ingood agreement with a model calculation [Fama, J, Shi, R.ABaragiola, Surface Sci., 602, 156 (2007)]. In the case of O2ice, O2+ has a significant lower sputtering yield whencompared to O+. The sputtering yields for O2 ice werefound to be at least 9 times larger compared to those forH2O ice. For H2O ice the sputter yields for C, N and O ionswere found to decrease with increasing mass. Doublycharged C, N and O ions which were found to have thesame sputtering yield as the singly charged ions within theexperimental errors. A preliminary TPD study was carriedout using a QMS to detect the desorbed species from waterice after irradiation by 6 × 10^15 ions of 13C+ and 13C2+.The formation of 13CO and 13CO2 was observed with theyield of 13CO almost of a factor of 100 larger than of13CO2. This is in contrast to our earlier work where onlyCO¬2 was observed. [A. Dawes et al., Phys. Chem. Chem.Phys., 9, 2886 (2007)].

Author(s): Elena Andra Muntean (Queen`s University Belfast), TomField (Queen`s University Belfast), Alan Fitzsimmons (Queen`s UniversityBelfast), Adam Hunniford (Queen`s University Belfast), Pedro Lacerda (MaxPlanck Institute for Solar System Research), Bob McCullough (Queen`sUniversity Belfast)

413.04 – Rotational Deexcitation of CO inInelastic Collisions with HCarbon monoxide, the second most abundant molecule inthe universe after molecular hydrogen, is found in a varietyof astrophysical environments and is typically observed inabsorption in the UV and near-IR and emission in theFIR/submm. The chemical and physical conditions whereCO resides are deduced from spectral lines, but it is oftennot appropriate to assume local thermodynamic equilibrium(LTE) in these regions. Therefore, collisional ratecoefficients with the dominant collision partners H, H2, andHe are necessary to accurately predict spectral lineintensities and extract astrophysical parameters. We reportnew quantum scattering calculations for rotationaldeexcitation transitions of CO induced by H using the newpotential energy surface(PES) of Song et al. (2013, J. Phys.Chem. A, 117, 7571). This highly sophisticated three-dimensional ab initio PES uses the spin-unrestrictedopen-shell single and double excitation coupled-clustermethod with perturbative triples [UCCSD(T)], withmolecular orbitals from restricted Hartree-Fock(RHF)calculations. State-to-state cross sections for collision

energies from 10-5 to 104 cm-1 and rate coefficients fortemperatures ranging from 1 to 3000 K are computed forCO(v=0, j) deexcitation from j=1-70 to all lower j' levels,where j is the rotational quantum number. The current ratecoefficients are compared with previous scattering resultsusing earlier PESs and the differences are discussed.Author(s): Kyle Walker (University of Georgia), Lei Song (RadboudUniversity Nijmegen), Benhui Yang (University of Georgia), GerritGroenenboom (Radboud University Nijmegen), Ad van der Avoird(Radboud University Nijmegen), Balakrishnan Naduvalath (UNLV), RobertForrey (Penn State Berks), Phillip Stancil (University of Georgia)

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414 – SPD Late PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

414.01 – Confined Eruption of a Multi-threadFilamentEruptive filaments are believed to be a major component,namely the core, of coronal mass ejections (CMEs). In`confined eruptions', the erupting materials eventuallycome back to the solar surface instead of escaping away.We study a multi-thread filament, within Active RegionNOAA 11861, that splits into two parts. The uppercomponent erupts and comes down while the lowercomponent remains almost in the same location. The dataset analyzed includes H$\alpha$ observation from the1-meter New Vacuum Solar Telescope (NVST) at YunnanAstronomical Observatory (YNAO) and the EUVobservations taken by the Atmospheric Imaging Assembly(AIA) onboard the Solar Dynamics Observatory (SDO). BothH$\alpha$ and EUV observations show the erupting phaseclearly. Fine details of the eruption are revealed by the highresolution and high cadence H$\alpha$ observations. Thegradual expansion of the filament is followed by twisting ofthreads that leads to a sudden eruption. The intuition ofthis process suggests a helical kink instability. Byextrapolating the vector magnetograms obtained byHelioseismic and Magnetic Imager (HMI) on SDO, wecalculate the magnetic twist and discuss if the kinkinstability plays a major role of initializing this eruption. Inaddition, we investigate the overlying fields, also known asstrapping fields, that confine against the eruptions. Thedecay index, a quantitative measurement of the strappingfields, is estimated to be 0.86. This value is smaller thanthe critical value of 1.5 indicating a strong strapping fieldpreventing the materials from escaping.Author(s): Yan Xu (New Jersey Institute of Tech.), Zhi Xu (YunnanAstronomical Observatory), Zhong Liu (Yunnan Astronomical Observatory),Rui Liu (University of Science and Technology of China), Chang Liu (NewJersey Institute of Tech.), Ju Jing (New Jersey Institute of Tech.), HaiminWang (New Jersey Institute of Tech.)

414.02 – Quick Time-dependent IonizationCalculations Depending on MHD SimulationsTime-dependent ionization is important in astrophysicalenvironments where the thermodynamic time scale isshorter than ionization time scale. In this work, we report aFORTRAN program that performs fast non-equilibriumionization calculations based on parallel computing. UsingMHD simulation results, we trace the movements of plasmain a Lagrangian framework, and obtain evolutionary historyof temperature and electron density. Then thetime-dependent ionization equations are solved using theeigenvalue method. For any complex temperature anddensity histories, we introduce a advanced time-stepstrategy to improve the computational efficiency. Our testsshow that this program has advantages of high numericalstability and high accuracy. In addition, it is also easy tointegrate this solver with the other MHD routines.Author(s): Chengcai Shen (Harvard-Smithsonian Center forAstrophysics), John Raymond (Harvard-Smithsonian Center forAstrophysics), Nicholas Murphy (Harvard-Smithsonian Center forAstrophysics)

414.03 – Two Categories of ApparentTornado-like ProminencesTwo categories of solar prominences have been describedin the literature as having a pattern of mass motions and/ora shape similar to terrestrial tornados. We first identify thetwo categories associated with prominences in the historicliterature and then show that counterparts do exist for bothin recent literature but one has not been called a tornadoprominence. One category described as being similar totornados is associated with the barbs of quiescent filamentsbut barbs appear to have rotational motion only underspecial conditions. H alpha Doppler observations from HelioResearch confirm that this category is an illusion in ourmind’s eye resulting from counterstreaming in the largebarbs of quiescent filaments. The second category is aspecial case of rotational motion occurring during the earlystages of some erupting prominences, in recent yearscalled the roll effect in erupting prominences. In thesecases, the eruption begins with the sideways rolling of thetop of a prominence. As the eruption proceeds the rollingmotion propagates down one leg or both legs of anerupting prominence depending on whether the eruption isasymmetric or symmetric respectively. As an asymmetriceruption proceeds, the longer lasting leg becomes nearlyvertical and has true rotational motion. If only this phase ofthe eruption was observed, as in the historic cases, it wascalled a tornado prominence and spectra recorded in thesecases provide proof of the rotational motion. When oneobserves an entire eruption which exhibits the rollingmotion, as accomplished at Helio Research, the similarity toa tornado is lost because the event as a whole has quite adifferent nature and the analogy to a terrestrial tornado notlonger appears suitable or helpful in understanding theobserved and deduced physical processes. Our conclusionis that there are no solar prominences with motions thatare usefully described as tornado or tornado-like eventsaside from the fun of observing some prominence barbswhose mass motions yield a fascinating illusion ofrotational motion under special conditions.Author(s): Sara Martin (Helio Research), AparnaVenkataramanasastry (University of North Dakota)

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414.04 – Fermi Detection of Gamma-rayEmission from a Behind-the-limb M1.5 Flareon 2013 October 11On 2013 October 11 an M1.5 class solar flare erupted fromthe NOAA active region 11868, which was then behind thesolar limb. RHESSI images reveal hard X-ray emission wellabove the limb, most likely from the top of the flare loopwhose footpoints were occulted. Surprisingly the FermiLarge Area Telescope (LAT) detected gamma-rays up to 3GeV for ~30 minutes from this flare, making it the firstbehind-the-limb flare observed by Fermi. The LATgamma-ray emission centroid is consistent with the vicinityof the RHESSI hard X-ray source. The gamma-ray spectracan be adequately described by a power law with ahigh-energy exponential cutoff, or as a result of the decayof pions produced by accelerated protons and ions with anisotropic pitch angle distribution and a power-law energyspectrum. The required proton spectrum would have anumber index of ~3.8. We present the Fermi and RHESSIobservations together with STEREO and SDO data toexplore the various emission scenarios of this behind-the-limb flare.Author(s): Melissa Pesce-Rollins (INFN), Nicola Omodei (KIPAC), VahePetrosian (KIPAC), Wei Liu (Lockheed Martin Solar and AstrophysicsLaboratory), Qingrong Chen (KIPAC), Fatima Rubio Da Costa (KIPAC)

Contributing teams: Fermi LAT Collaboration

414.05 – SWARM: A Compact HighResolution Correlator and Wideband VLBIPhased Array Upgrade for SMAA new digital back end (DBE) is being commissioned onMauna Kea. The “SMA Wideband Astronomical ROACH2Machine”, or SWARM, processes a 4 GHz usable band insingle polarization mode and is flexibly reconfigurable for 2GHz full Stokes dual polarization. The hardware is based onthe open source Reconfigurable Open ArchitectureComputing Hardware 2 (ROACH2) platform from theCollaboration for Astronomy Signal Processing andElectronics Research (CASPER). A 5 GSps quad-core analog-to-digital converter board uses a commercial chip from e2vinstalled on a CASPER-standard printed circuit boarddesigned by Homin Jiang’s group at ASIAA. Two ADCchannels are provided per ROACH2, each sampling a 2.3GHz Nyquist band generated by a custom wideband blockdownconverter (BDC). The ROACH2 logic includes16k-channel Polyphase Filterbank (F-engine) per inputfollowed by a 10 GbE switch based corner-turn which feedsinto correlator-accumulator logic (X-engines) co-locatedwith the F-engines. This arrangement makes very effectiveuse of a small amount of digital hardware (just 8 ROACH2sin 1U rack mount enclosures). The primary challenge now isto meet timing at full speed for a large and very complexFPGA bit code. Design of the VLBI phased sum and recorderinterface logic is also in process. Our poster will describethe instrument design, with the focus on the particularchallenges of ultra wideband signal processing. Earlyconnected commissioning and science verification data willbe presented.Author(s): Jonathan Weintroub (Harvard-Smithsonian Center forAstrophysics)

Contributing teams: The SWARM Development Team

414.06 – MOSES Inversions usingMultiresolution SMARTWe present improvements to the SMART inversionalgorithm for the MOSES imaging spectrograph. MOSES, theMulti-Order Solar EUV Spectrograph, is a slitless extremeultraviolet spectrograph designed to measure cotemporalnarrowband spectra over a wide field of view viatomographic inversion of images taken at three orders of aconcave diffraction grating. SMART, the SmoothMultiplicative Algebraic Reconstruction Technique, relies ona global chi squared goodness of fit criterion, which enablesoverfit and underfit regions to "balance out" when judgingfit quality. "Good" reconstructions show poor fits at somepositions and length scales. Here we take a multiresolutionapproach to SMART, applying corrections to thereconstruction at positions and scales where correction iswarranted based on the noise. The result is improved fitresiduals that more closely resemble the expected noise inthe images. Within the multiresolution framework it is alsoeasy to include a regularized deconvolution of theinstrument point spread functions, which we do. Differentpoint spread functions among MOSES spectral ordersresults in spurious doppler shifts in the reconstructions,most notable near bright compact emission. We estimatethe point spread funtions from the data. Deconvolution isdone using the Richardson-Lucy method, which isalgorithmically similar to SMART. Regularization results fromonly correcting the reconstruction at positions and scaleswhere correction is warranted based on the noise. Weexpect the point spread function deconvolution to increasesignal to noise and reduce systematic error in MOSESreconstructions.Author(s): Thomas Rust (Montana State University), Lewis Fox(National Solar Observatory), Charles Kankelborg (Montana StateUniversity), Hans Courrier (Montana State University), Jacob Plovanic(Montana State University)

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415 – Education and Public Outreach PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

415.01 – A Low-cost 21 cm Horn-antennaRadio Telescope for Education and OutreachSmall radio telescopes (1-3m) for observations of the 21 cmhydrogen line are widely used for education and outreach.A pyramidal horn was used by Ewen & Purcell (1951) to firstdetect the 21cm line at Harvard. Such a horn is simple todesign and build, compared to a parabolic antenna which isusually purchased ready-made. Here we present a design ofa horn antenna radio telescope that can be built entirely bystudents, using simple components costing less than $300.The horn has an aperture of 75 cm along the H-plane, 59cm along the E-plane, and gain of about 20 dB. Thereceiver system consists of low noise amplifiers, band-passfilters and a software-defined-radio USB receiver thatprovides digitized samples for spectral processing in acomputer. Starting from construction of the horn antenna,and ending with the measurement of the Galactic rotationcurve, took about 6 weeks, as part of an undergraduatecourse at Harvard University. The project can also growtowards building a two-element interferometer for follow-upstudies.Author(s): Nimesh Patel (Harvard-Smithsonian Center forAstrophysics), Rishi Patel (Massachusetts Institute of Technology), RobertKimberk (Harvard-Smithsonian Center for Astrophysics), John Test(Harvard-Smithsonian Center for Astrophysics), Alex Krolewski (HarvardUniversity), James Ryan (Harvard University), Kirit Karkare (Harvard-Smithsonian Center for Astrophysics), John Kovac (Harvard University),Thomas Dame (Harvard-Smithsonian Center for Astrophysics)

415.02 – Measuring the CMB temperature inthe classroom with a low-cost antenna andradiometerEstimation of the cosmic microwave background (CMB)temperature through a skydip is an ambitiousundergraduate laboratory exercise in which care must betaken to understand and account for systematic errors. It isan ideal environment for learning about carefulexperimental design. We present two versions of a low-costantenna and radiometer system replicating the CMBdiscovery measurement (Penzias and Wilson, 1965),operating at 11 and 19 GHz. We describe two small-aperture (8") antenna designs: an HDPE lens-coupledcorrugated horn, and a single-groove Potter horn, both ofwhich are simple and inexpensive to fabricate. They havebeen designed to minimize far sidelobe pickup from theground in conjunction with a straight-walled or Winstoncone. The radiometers are based on low-cost commercialsatellite TV receivers, read out with standard laboratoryequipment. We describe the design of aperture-fillingcalibration loads necessary to characterize the radiometerperformance. Several iterations of this experiment havebeen run in the advanced undergraduate astrophysicslaboratory course (Ay 191) at Harvard University, with thestudents building the apparatus starting from scratch andfinishing in about 6 weeks. Positive detections ofbackground radiation have been achieved with typicaluncertainties of 0.3 K.Author(s): Kirit Karkare (Harvard-Smithsonian Center forAstrophysics), Rachel Bowens-Rubin (Harvard-Smithsonian Center forAstrophysics), Jake Connors (Harvard-Smithsonian Center forAstrophysics), Thomas Dame (Harvard-Smithsonian Center forAstrophysics), Ryan Gao (Harvard-Smithsonian Center for Astrophysics),Samuel Harrison (Harvard-Smithsonian Center for Astrophysics), RobertKimberk (Harvard-Smithsonian Center for Astrophysics), John Kovac(Harvard-Smithsonian Center for Astrophysics), Jamie Law-Smith (Harvard-Smithsonian Center for Astrophysics), Derek Robins (Harvard-SmithsonianCenter for Astrophysics), Steve Sansone (Harvard-Smithsonian Center forAstrophysics), Robert Wilson (Harvard-Smithsonian Center forAstrophysics), Anya Yermakova (Harvard-Smithsonian Center forAstrophysics), Lingzhen Zeng (Harvard-Smithsonian Center forAstrophysics)

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415.03 – Students’ Attitudes andUnderstandings about Science in their FieldTrip to Laser InterferometerGravitational-wave Observatory (LIGO)The LIGO Science Education Center in Livingston, LA,provides K-12 students with 3.5-hour field trip programsthat consist of watching a documentary, touring the LIGOfacilities, exploring interactive science exhibits, andhands-on classroom activities with the Center’s staff. In ourstudy we administered a pre/post-survey, which consistedof Likert-type and open-ended questions, to approximately1,000 secondary students who visited LIGO in Spring 2013.In this paper we report on our current findings from ahalf-way analysis about 1) the students’ attitudes andinterests about science; 2) their understanding about basicscientific concepts relevant to LIGO science, gravity, light,and sound; and 3) their understanding about the LIGOproject. In comparison between pre and post-responsesusing a paired-samples t-test, the results showed that thefield trip to LIGO had significant (p<0.05) positive impacton increasing the number of students who think that"science is fun" and that they "would want to be a

scientist." In addition, they had significant (p<0.05)knowledge gain in understanding that there are frequenciesof light that are not visible, and they were able to correctlyname the different kinds of electromagnetic waves after thevisit. In pre-test 51.5% responded that they did not evenhear about LIGO and 17.8% could not explain what it wasalthough they heard about it (as they were from the localschools). On the other hand, 86.6% students were able toexplain about LIGO project in post-test. Among them, morethan half of the students (59.3%) correctly described thepurpose of the LIGO project. Another 9.3% recognized it asa science research center without further information aboutwhat specifying the purpose of LIGO. About 8% heldmisconceptions, and 7% recognized LIGO as a sciencelearning center. The students’ learning in this field triphappened mainly by: encountering the new concept;recalling their prior knowledge and reinforcing it; and beingable to connect the scientific concept to how it is applied ina professional science research.Author(s): Hyunju Lee (University of South Florida), Allan Feldman(University of South Florida)

Contributing teams: LIGO Livingston Science EducationCenter

416 – Extrasolar Planets PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

416.01 – Tidal Alignment of ExoplanetsAround Low Mass StarsUsing the Rossiter-McLaughlin effect, the projectedspin–orbit angle for many exoplanetary systems has nowbeen measured. Thanks to this rapidly increasing sample itis becoming clear that stars with surface convective zonesappear to be well aligned while those without span a widerange of inclinations. The explanation proposed (Winn et al2010) is that perhaps only the convective zones align withthe planet, while the cores remain misaligned. Thisexplanation suffers from two problems however: thecore-envelope coupling in low mass stars appears to bestrong enough to prevent long-lived differential rotation andeven if only the convective zone is aligned, the planetgenerally does not survive for long after that. Since tidesdue to a planet on a misaligned orbit have a component atthe rotational frequency of the star, and for an alignedplanet the only frequency is the difference between thegenerally fast planet and the slowly rotating star, it isconceivable that misaligned systems are subject to muchenhanced dissipation, acting for example on resonantlyexcited inertial waves in the star. However, Rogers & Lin(2013) point out that under inertial mode dissipation, inaddition to aligned orbits one would expect a pile-up onpolar and/or exactly counter-rotating orbits. We proposethat the extra equilibrium solutions disappear if oneincludes in the evolution the fact that stars evolve and shedangular momentum throughout their lifetime. We have builta model including all those effects and will show resultsexploring this explanation.

Author(s): Kaloyan Penev (Princeton University), Brian Jackson(Carnegie Dept. of Terrestrial Magnetism)

416.02 – Colour Magnitude Diagrams ofTransiting ExoplanetsColour-Magnitude diagrams form a traditional way ofrepresenting luminous objects in the Universe and comparethem to each others. Here, the photometric distances of 44transiting exoplanetary systems were estimated. For sevenof those, parallaxes confirm the methodology. From thecombination of those measurements with fluxes obtainedwhile planets were occulted by their host stars, colour-magnitude diagrams are composed in the near and mid IR.When possible, planets are plotted with field brown dwarfswho often have similar sizes and equilibrium temperatures,thus offering a natural empirical comparison sample.Exoplanets are also compared to the expected loci of pureblackbodies. In general planets do not agree with the browndwarfs sequences, and neither do they match blackbodies.It is however possible to affirm that they are not featurelessand that they display an increasing diversity in colour withdecreasing intrinsic luminosity. A missing source ofabsorption within the [4.5 ?m] band, for some planets,would generally reconcile hot Jupiters with brown dwarfs’cool atmospheres. Alternatively, measuring the emission ofgas giants cooler than 1 000 K would disentangle whetherplanets’ atmospheres behave like brown dwarfs’atmospheres, like blackbodies, or whether they form theirown sequence.Author(s): Amaury Triaud (Massachusetts Institute of Technology)

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417 – Galaxies Near and Far PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

417.01 – The Galactic Center Radio Arc: AMulti-Frequency Spectro-Polarimetric StudyDespite the Radio Arc non-thermal filaments (NTFs) beingdiscovered 30 years ago, their origin remain poorlyunderstood. The Radio Arc NTFs have an unusually flatspectrum in the centimeter to millimeter spectrum with apredicted, though poorly constrained, turn-over between30- 200 GHz. With the recently upgraded wide-bandcapabilities of the VLA, we conducted a multi-frequencyspectro-polarimetric study of the Radio Arc region. Withobservations at a set of low radio frequencies (continuouscoverage over 2-6 GHz & 10-12 GHz), we imaged both thetotal and polarized intensity distributions at high angularresolution (? 1”). Presented here are the preliminary resultsfrom four observations spanning May 2013 to February2014 using the DnC, CnB, B & BnA array configurations.This study has produced the deepest continuum intensityimages of the Radio Arc region to date, with a sensitivity anorder of magnitude greater than previous surveys, andresulted in the detection of new structure and compactemission sources. These observations will serve as a pilotpolarization study for larger, more complete polarimetricsurveys of the Galactic center region.Author(s): James Toomey (University of Iowa), Cornelia Lang(University of Iowa), Dominic Ludovici (University of Iowa)

417.02 – Are The Known Milky WaySatellites Enough?We study the past orbital history of the classical Milky Waysatellites, by integrating backwards from their observedpositions and proper motions. Starting from the initialconditions derived from the proper motions, we examinethe tidal effect of all the known classical Milky Waysatellites on the galactic disk. We sample the largeparameter space of the measured proper motions andassociated uncertainties by modeling the galactic disk ascomposed of test particles. This approach allows us toquantify the effect of the orbital distribution on the galacticdisk, and provide realistic initial conditions for the classicalMilky Way satellites. We show that the main tidal players ofthe Milky Way are the Sagittarius (Sgr) dwarf galaxy, theLarge Magellanic Cloud (LMC), and the Small MagellanicCloud (SMC). We examine both the vertical and planardisturbances of the galactic disk. We show that the Sgrdwarf is the primary culprit responsible for producing thewarp of the galactic disk. However, we find that the planardisturbances excited by all the eleven classical satellites(which closely matches the response due to the three maintidal players) is a factor of ~ 85 lower than what is requiredto explain the amplitude of the observed disturbances inthe outer HI disk of the Milky Way. Thus, while the verticalstructure of the galactic disk may be explained by theknown satellites, the radial motions generated by theknown Milky Way satellites are far less than what isrequired to explain the observed data. This largediscrepancy of nearly two orders of magnitude between theobserved planar disturbances and that produced by all theknown classical satellites suggests that putative, newsatellites (such as the one predicted by Chakrabarti & Blitz2009) may be necessary to explain the observations.Author(s): Sukanya Chakrabarti (Rochester Institute ofTechnology), Alice Quillen (University of Rochester), Philip Chang(University of Wisconsin-Milwaukee)

417.03 – Chandra Galaxy AtlasThe hot ISM in early type galaxies plays a crucial role forunderstanding their formation and evolution. Structuralfeatures of the hot ISM identified by Chandra (includingjets, cavities, cold fronts, filaments and tails) point to keyevolutionary mechanisms, e.g., AGN feedback, merginghistory, accretion/stripping and star formation and itsquenching. In our new project, Chandra Galaxy Atlas, wewill systematically analyze the archival Chandra data of137 ETGs to study the hot ISM. Taking full advantage of theChandra capabilities, we will derive uniform data productsof spatially resolved dataset with additional spectralinformation. We will make these products publicly availableand use them for our focused science goals.Author(s): Dong-Woo Kim (Harvard-Smithsonian, CfA), AmyMossman (Harvard-Smithsonian, CfA), Antonella Fruscione (Harvard-Smithsonian, CfA), Craig Anderson (Harvard-Smithsonian, CfA), DougMorgan (Harvard-Smithsonian, CfA), Douglas Burke (Harvard-Smithsonian,CfA), E. O'Sullivan (Harvard-Smithsonian, CfA), Giuseppina Fabbiano(Harvard-Smithsonian, CfA), Jennifer Lauer (Harvard-Smithsonian, CfA),Mike McCollough (Harvard-Smithsonian, CfA)

417.04 – Parsec-Scale Radio JetCharacteristics of MOJAVE Hard-SpectrumGamma-Ray BlazarsMOJAVE is a long term VLBA key project to probe thestructure and evolution of parsec-scale radio jetsassociated with active galactic nuclei (AGN). Our programhas found that apparent superluminal motion is common incompact radio-selected AGN, indicating Lorentz factors upto ~50 in outflows oriented at a few degrees from the lineof sight. Recently we have begun regularly obtaining 2 cmVLBA full polarization images of a new AGN sampleselected on the basis of hard-spectrum gamma-ray flux.Only about 10% of these AGN have previously beenmonitored with VLBA, and they show slow apparent jetspeeds that appear to be inconsistent with the very highDoppler factors inferred from emission modelling and rapidvariability at high photon energies. We discuss thefirst-epoch radio jet properties of our sample, and thedetection of superluminal motion in the jet associated withthe hard-spectrum TeV blazar 1ES 1011+496.Author(s): Matthew Lister (Purdue Univ.)

Contributing teams: The MOJAVE Collaboration

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417.05 – Variability of the radio-loud NLS1galaxy PKS 0558-504We carried out photometric studies of the radio-loudNarrow-line Seyfert 1 galaxy (NLS1) PKS0558-504 usingboth the first Antarctic Survey Telescope (AST3-1, 0.5 maperture) located at Dome A in Antarctica and the 0.6 mSoutheastern Association for Research in Astronomy (SARA)South telescope located at the Cerro Tololo Inter-AmericanObservatory in Chile. The AST3-1 telescope is equippedwith a 10K×10K single-chip CCD camera, which is one ofthe largest single-chip CCD cameras ever used inastronomy, and its site provides the best observationconditions on earth’s surface. The photometric data takenwith AST3-1 were obtained with cousin i band during 6nights from April 30 to May 7, 2012. In order to compareand double check the data quality, this target was imagedagain using the SARA 0.6 m telescope with SDSS-g and ibands during 10 nights from October 31 to December 16,2012. We will present detailed data analyses, the lightcurves obtained from both telescopes, and the mechanismfor the light variability.Author(s): Xianming Han (Butler University), QiGuo Tian (PolarResearch Institute of China), Tuo Ji (University of Science and Technologyof China), WenJuan Liu (University of Science and Technology of China),HongYan Zhou (University of Science and Technology of China)

417.06 – UVUDF: Ultraviolet Imaging of theHubble Ultra Deep Field with Wide-FieldCamera 3We present recent science results from the UltravioletCoverage of the Hubble Ultradeep Field (UVUDF) project, inwhich we obtained images of the HUDF with WFC3/UVIS inthe F225W, F275W, and F336W filters (30 orbits per filter;half with UVIS post-flash). The UVUDF completes theHubble Space Telescope wavelength coverage of the moststudied field in the extragalactic sky in the major imagingbands (FUV through NIR). As illustrated by a new 13-bandimage of the HUDF, these data give us the best view yetobtained of the last 9-10 billion years of cosmicstar-formation. The UVUDF data enable the analysis ofstar-forming galaxies at z~2 (Lyman break galaxies at thepeak era of star formation) that would be inaccessible fromthe ground, including measurement of the slope of their UVcontinuum. The high spatial resolution of the UVUDFimages are an unprecedented resource for studying the UVstructure of galaxies at z~1 and understanding howgalaxies are formed from clumps of hot stars.Author(s): Harry Teplitz (Caltech), Marc Rafelski (Caltech), PeterKurczynski (Rutgers University), Nicholas Bond (GSFC), Emmaris Soto(CUA), Norman Grogin (STScI), Anton Koekemoer (STScI), Hakim Atek(EPFL), Thomas Brown (STScI), Dan Coe (STScI), James Colbert (Caltech),Yu Dai (Caltech), Henry Ferguson (STScI), Steven Finkelstein (UT Austin),Jonathan Gardner (GSFC), Eric Gawiser (Rutgers University), MauroGiavalisco (U. Mass.), Caryl Gronwall (Penn State), Daniel Hanish (Caltech),Kyoung-Soo Lee (Purdue), Zoltan Levay (STScI), Duilia De Mello (CUA),Swara Ravindranath (STScI), Russell Ryan (STScI), Brian Siana (UCRiverside), Claudia Scarlata (UMN), Elysse Voyer (CNRS), Rogier Windhorst(ASU)

417.07 – SuperBIT: Wide-field,Sub-arcsecond Imaging from the SuperPressure Balloon PlatformThe scientific potential of near-diffraction-limited imagingfrom mid-latitude ultra-long duration balloon payloads iswell known. The combination of diffraction-limited angularresolution, extreme stability, space-like backgrounds, andlong integrations enables transformative opportunities instudies ranging from the weak lensing of galaxy clustersand cosmic shear to the search for exoplanets.Collaborators at the University of Toronto have recentlyintegrated a half-meter class telescope with a prototypesubarcsecond pointing system. SuperBIT will adapt theexisting system to the requirements of the mid-latitudesuper-pressure balloon (SPB) payload, and demonstrate itsimaging capability during an ultra-long duration balloonflight that will take off from Wanaka, New Zealand, in the2016-17 Austral summer. The demonstration instrumentwill provide imaging with a half-degree field of view and0.3-arcsecond resolution in five bands between 300 and1000 nm, with sensitivities in the shape-band exceeding24th magnitude (>5 sigma) in 300 seconds of integration.Our observing schedule will be split between a performanceverification sample, a photometric and spectroscopiccalibration set, a deep field, and a science catalog. Theperformance verification set prioritizes a sample of thirtyclusters that have been previously well studied with theHST Advanced Camera for Surveys, the Chandra X-rayobservatory, and for which there are Compton-Y parameterdata from millimeter-wavelengths. The photometriccalibration set will be selected from the COSMOS field. Thescience catalog will draw from a set of more than 150Sunyaev-Zel’dovich, X-ray, and optically selected clustersspanning a wide range of cluster masses and morphologies.Aside from demonstrating the technical approach, thesedata will enable a systematic program to constrain themass-observable relations over an unprecedented scale. Asuccessful demonstration of the technical approach and thescientific potential will motivate future development offacility-class instruments on the SPB platform.Author(s): Jason Rhodes (JPL), Aurélien Fraisse (Princeton), WilliamJones (Princeton), Calvin Barth Netterfield (University of Toronto), RichardMassey (Durham)

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417.08 – Molecular Gas in the Cooling FlowGroup NGC 5044 as Revealed by ALMAAn ALMA observation of the early-type galaxy NGC 5044,which resides at the center of an X-ray bright group with amoderate cooling flow, has detected 24 molecularstructures within the central 2.5 kpc. The masses of themolecular structures vary from 3e5 Mo to 1e7 Mo and theCO(2-1) linewidths vary from 15 to 65 km/s. Given the largeCO(2-1) linewidths, the observed structures are likely giantmolecular associations (GMAs) and not individual molecularclouds (GMCs). Only a few of the GMAs are spatiallyresolved and the average density of these GMAs yields aGMC volume filling factor of about 15%. The observedmasses of the resolved GMAs are insufficient for them to begravitationally bound, however, the most massive GMAdoes contain a less massive component with a linewidthtypical of an individual virialized GMC. There are noindications of any disk-like molecular structures and allindications suggest that the molecular gas follows ballistictrajectories after condensing out of the thermally unstablehot gas. The 230 GHz luminosity of the central continuumsource is 500 times greater than its low frequency radioluminosity and probably reflects a recent accretion eventby the central AGN. The spectrum of the central AGN alsoexhibits an absorption feature with a linewidth typical of anindividual GMC and an infalling radial velocity of 250 km/s.Author(s): Laurence David (Harvard Smithsonian, CfA), Jeremy Lim(University of Hong Kong), William Forman (Harvard Smithsonian, CfA), JanVrtilek (Harvard Smithsonian, CfA), Francoise Combes (Observatoire deParis), Philippe Salome (Observatoire de Paris), Alastair Edge (DurhamUniversity ), Ming Sun (University of Alabama), Fabio Gastaldello (INAF),Pasquale Temi (NASA/Ames), Henrique Schmitt (NRL), Youichi Ohyama(Institute of Astonomy and Astrophysics), Steven Hamer (DurhamUniversity ), William Mathews (University of California Santa Cruz), Fabrizio

Brighenti (Universit di Bologna), Simona Giacintucci (University ofMaryland), Sandro Bardelli (NRL), Dinh-V Trungg (Vietnamese Academy ofScience and Technology)

417.09 – Star Formation and Cooling inCLASH Brightest Cluster GalaxiesWe present new constraints on star-formation in thebrightest cluster galaxies (BCGs) of the 20 X-ray selectedCLASH galaxy clusters. Using 16 HST passbands, we findevidence for significant UV and H? +[NII] emission in ? 50%of these intermediate redshift (? 0.2 - 0.6) BCGs. Theemission appears to come from regions withmorphologically irregular knots and filaments. The UV andH? fluxes are well correlated with one another. Theextinction-corrected luminosities are consistent with theKennicutt law for continuous star formation. For the largestemission structures we observe, we estimate that the SFRsare 100-200 Msun yr?1, under the assumption that the UVand H? emission is solely due to star formation. Wehypothesize that the structures we observe are either directfeatures of a cooling mechanism in the cores of theseclusters or are a direct consequence of the processes thatregulate the cooling. Using data from the ACCEPT catalog ofChandra observations of these clusters, we find acorrelation between the UV luminosity and several X-rayderived ICM properties. In particular, we find a possiblescaling between either the UV or H?+[NII] luminosity andthe 1 Gyr cooling radius. These UV and H? features aresurprisingly prevalent in the CLASH sample and this newstudy provides us with new constraints on the physics ofgas flows and star formation in cluster cores.Author(s): Kevin Fogarty (Johns Hopkins University), Marc Postman(Space Telescope Science Instiitute), Megan Donahue (Michigan StateUniversity), John Moustakas (Siena College)

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418 – Instrumentation PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

418.01 – Distorted Noise Properties of HSTACS/WFC Images after Pixel-basedCorrection for Poor Charge-transferEfficiencyThe HST Advanced Camera for Surveys (ACS) imagecalibration pipeline, CALACS, now performs a pixel-basedcorrection for the Wide Field Camera’s (WFC) imperfect CCDcharge transfer efficiency (CTE). The degradation of theWFC CTE has become severe in recent years, requiring acorrespondingly more aggressive correction inpost-processing. This correction may be described as aspatially variable deconvolution, and unavoidably distortsthe pixel-to-pixel noise properties of WFC images incomplex ways that have not yet been fully quantified. Thecurrent study addresses this lack of knowledge byinvestigating the pixel variance and correlated noise incontrol samples of processed calibration files spanning theoperational lifetime of ACS. We choose two cases ofextreme CTE losses, due to their low backgrounds: 1)1000-second dark frames (heavy contamination fromcosmic rays and CCD hot pixels); and 2) bias frames (onlycontamination from cosmic rays during readout). In bothcases, we spoof the CALACS pipeline into treating thecalibration exposures as dithered science images, for themost faithful replication of the noise propertiesencountered by the typical WFC observer who stacksdithered exposures. The results of the analyses presentedhere will refine the CALACS-generated pixel error array thataccompanies the calibrated science image.Author(s): Josh Sokol (STScI), Norman Grogin (STScI)

418.02 – Development of Off-PlaneReflection Grating Alignment FixturesCurrently, grating spectrometers are used onboard theChandra X-ray Observatory and XMM-Newton in orbitaround the Earth. However, future goals of greater spectralresolving power and greater effective areas necessitate anew generation of high-quality spectrometers. Off-planereflection gratings can be used to provide high throughputand spectral resolution in the 0.3-2.0 keV band, allowing forunprecedented diagnostics of energetic astrophysicalprocesses. A grating spectrometer consists of multiplealigned gratings intersecting the converging beam of aWolter-I telescope. Each grating will be aligned such thatthe diffracted spectra overlap at the focal plane.Misalignments will degrade both spectral resolution andeffective area. With analytical alignment tolerancescalculated, laboratory techniques to achieve thesetolerances for flight-like optics must be developed. Wepresent the results from our first and second generationalignment fixtures, as well as wavefront stitching methods.Author(s): Benjamin Donovan (University of Iowa), Ryan Allured(Harvard-Smithsonian Center for Astrophysics), Randall McEntaffer(University of Iowa)

418.03 – FIFI-LS - The Facility Far-InfraredSpectrometer for SOFIAFIFI-LS is the German far-infrared integral fieldspectrometer for the SOFIA airborne observatory. Theinstrument offers medium resolution spectroscopy (R ~ afew 1000) in the far-infrared with two independentspectrometers covering 45-110um and 100-210um. Theintegral field units of the two spectrometers obtain spectracovering concentric square fields-of-views sized 30" and60", respectively. Both spectrometers can observesimultaneously at any wavelength in their ranges makingefficient mapping of far-infrared lines possible. FIFI-LS isbeing commissioned at the airborne observatory SOFIA firstas a PI instrument in spring 2014. During 2015, thecommissioning as facility instrument will be complete andthe SOFIA observatory will take over the operation ofFIFI-LS. The instrument can already be used by thecommunity. Primary science cases are the study of thegalactic and extra-galactic interstellar medium and starformation. The capabilities of FIFI-LS on the SOFIAtelescope and observing modes will be explained. FIFI-LSoffers observing modes for compact sources, extendedsources, and mapping. All modes use spatial and spectraldithering. The resulting data products will be 3D-datacubes. The spectral extent will vary between 500km/s and2500km/s depending on the observing wavelength. Theobserving parameters will be specified using AOTs, like theother SOFIA instruments, and created via the tool SSPOTwhich is similar to the Spitzer Space Telescope SPOT tool.The observations will be done in service mode, but SOFIAinvites a few investigators to fly onboard SOFIA during (partof) their observations. After a flight, the data get pipelinereduced, quality checked by the SOFIA science staff, andprovided to the investigator via the SOFIA data archive.Author(s): Randolf Klein (USRA-SOFIA), Simon Beckmann (UniversityStuttgart), Aaron Bryant (University Stuttgart), Sebastian Colditz(University Stuttgart), Christian Fischer (University Stuttgart), Fabio Fumi(University Stuttgart), Norbert Geis (MPE), Rainer Hönle (UniversityStuttgart), Alfred Krabbe (University Stuttgart), Leslie Looney (UIUC),Albrecht Poglitsch (MPE), Walfried Raab (MPE), Felix Rebell (UniversityStuttgart), Maureen Savage (USRA-SOFIA)

418.04 – First Light with the EXESInstrument on SOFIAThe Echelon Cross Echelle Spectrograph (EXES)successfully carried out its first two flights with theStratospheric Observatory for Infrared Astronomy (SOFIA)on the nights of April 7 and 9, 2014. EXES is ahigh-resolution (R=100,000) spectrograph that operatesfrom 4.5 to 28.3 microns. Our commissioning targetsincluded a mix of solar system and Galactic objects whichwere selected to characterize the performance of EXESonboard SOFIA as well as to provide unique science data.We present some of these high-resolution spectra and thepreliminary science analysis, as well as our currentcharacterization of the on-sky performance and sensitivityof EXES.Author(s): Curtis DeWitt (NASA Ames), Matthew Richter (UC Davis),Kristin Kulas (NASA Ames), Mark McKelvey (NASA Ames), Michael Case (UCDavis), Robert McMurray (NASA Ames), William Vacca (Universities SpaceResearch Association), Melanie Clarke (Universities Space ResearchAssociation), Adwin Boogert (Universities Space Research Association),Graham Harper (Trinity College), Thomas Greathouse (Southwest ResearchInstitute), Nils Ryde (Lund University)

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418.05 – The 20-20-20 Airship ChallengeA NASA Centennial Challenge; (http://www.nasa.gov/directorates/spacetech/centennial_challenges/index.html)is in development to spur innovation in stratosphericairships as a science platform. We anticipate a million dollarclass prize for the first organization to fly a powered airshipthat remains stationary at 20km (65,000 ft) altitude forover 20 hours with a 20kg payload. The design must bescalable to longer flights with more massive payloads. InNASA’s constrained budget environment, there are fewopportunities for space missions in astronomy and Earthscience, and these have very long lead times. We believe

that airships (powered, maneuverable, lighter-than-airvehicles) could offer significant gains in observing time, skyand ground coverage, data downlink capability, andcontinuity of observations over existing suborbital optionsat competitive prices. We seek to spur private industry (ornon-profit institutions, including FFRDCs and Universities)to demonstrate the capability for sustained airship flightsas astronomy and Earth science platforms. This poster willintroduce the challenge in development and provide detailsof who to contact for more information.Author(s): Alina Kiessling (JPL), Ernesto Diaz (JPL), Sarah Miller (UCIrvine), Jason Rhodes (JPL)

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419 – Molecular Clouds, the ISM and YSOs PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

419.01 – H2 in the UV-rich Environment ofOrion's VeilUnderstanding the physics of molecular gas, almost bydefinition, requires understanding the physics of molecularhydrogen. H2 is the most abundant molecule in molecularclouds, the formation of H2 initiates the transition fromwarmer atomic to cooler molecular gas, and H2 serves as acatalyst in the formation of other molecules like CO that arewidely used to study star-forming regions. It is noexaggeration to say that a fundamental understanding ofthe earliest phases of star formation is impossible without afundamental understanding of the physics of H2. In thispresentation, we will present high-resolution UV absorptionspectroscopy towards the Trapezium stars in the OrionNebula. Using the STIS E140H setting of HST, we now havean S/N = 50 - 150 spectral dataset between 1133 - 1335Angstroms, with a spectral resolution of 2.5 km/s. Thisdataset will allow us to determine the H2 column density ina PDR which has a very low H2 column density (H2/H(tot) <10^-5). By observing the column density of highrotational/vibrational levels of H2, and combining theobservations a detailed model of ISM physics using Cloudy,we hope to better understand the physics of H2 in high-UVflux environments, which has applications to star-formingenvironments at the galactic and extra-galactic level.Author(s): Nicholas Abel (University of Cincinnati, ClermontCampus), Gary Ferland (University of Kentucky), C. O'Dell (VanderbiltUniversity), Thomas Troland (University of Kentucky)

419.02 – TRAO Outer Galaxy Survey in 13COWe present a result of 13CO(1-0) survey toward the OuterGalactic Plane using the multi-beam receiver systeminstalled on the 14 m telescope at Taeduk Radio AstronomyObservatory(TRAO). Our target region is from l=120o to140o and b=-1o to +1o, which is the part of the 12COOuter Galactic Plane Survey (Heyer et al. 1998). All dataare on 50" grid, and the beamsize is also 50". Velocityresolution is 0.63 km/sec, and the total velocity range isfrom -150 km/sec to 100 km/sec. A total of 23,000 spectrawere obtained. The rms noise is about 0.15 K per channelfor unsmoothed raw data. We will present a few initialresults of the survey database, comparing with 12CO OuterGalactic Plane Survey database.Author(s): Youngung Lee (Korea Astronomy and Space ScienceInstitute)

419.03 – Limits on the OVII Emission fromthe Local Hot BubbleConstraining the properties of the gas in the localhot-bubble (LHB) is important for the understanding of theinterstellar medium surrounding the sun. Much informationabout its energetic state is embedded in the observationsof the low-energy diffuse X-ray background. Frommolecular-cloud shadowing observations (Galeazzi et al.2006, R. Smith et al. 2007, Henley et al. 2007) it is knownthat a significant fraction of the 0.57keV OVII X-ray fluxoriginates locally (< ~300 pc). To investigate the origin ofthis OVII emission, we analyze the correlation between OVIIflux (extracted from Suzaku observations cleaned of pointsources) against the local fraction of the ROSAT ¼ keVemission (R12 band), as separated from the distant (hothalo/extragalactic) component by Snowden (1998) andKuntz (2000). Observations were selected to avoid galacticin-plane emission and features of other large-scale ISMstructures. After correcting OVII flux for the more distantlatitude-dependent emission, we find that it is essentiallyuncorrelated with the local ¼ keV emission, implying thatthe local hot bubble is not the source of the observed OVIIemission. The lack of OVII emission further precludestemperatures above ~1E6K for the LHB gas (assumingcollisional equilibrium models with solar abundance).Author(s): Felix Jaeckel (University of Wisconsin - Madison),Yaqiong Li (University of Wisconsin - Madison), Kelsey Morgan (Universityof Wisconsin - Madison), Natalia Petre (University of Wisconsin - Madison),Patrick Sauter (University of Wisconsin - Madison), Dan McCammon(University of Wisconsin - Madison)

419.04 – High Amlitude Near-InfraredVariability Among YSOs in the ONCWe have carried out deep, comprehensive NIR time-seriesobservations of the Orion Nebula Cluster using WFCAM onUKIRT, in an 0.9 x 0.9 degree J, H, K survey comprising~100 nights in a ~900 day window. Out of 14,728monitored objects brighter than J~20.5, we find 1202 highlyvariable stars with a Stetson variability index exceeding1.0, including 539 periodic sources with periods between 2and 50 days. We have calculated variability propertiesseparately for Class I, II, and III objects, and find thatClasses I and II have statistically larger amplitudevariability than Class III stars. Many stars have significantlyvariable J-H and H-K color terms; most of the Class II color-variables show color changes that are consistent withchanges in dust reddening, but a substantial fraction showcolor changes that indicate changes in accretion rate oraccretion structure.Author(s): Scott Wolk (Harvard-Smithsonian Center forAstrophysics), Thomas Rice (University of Michigan ), Bo Reipurth(University of Hawaii)

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419.05 – YSOVAR: Mid-IR variability in thestar forming region Lynds 1688The emission from young stellar objects (YSOs) in themid-IR is dominated by the inner rim of their circumstellardisks. We present an IR-monitoring survey in the directionof the Lynds 1688 (L1688) star forming region over fourvisibility windows spanning 1.6 years using the Spitzerspace telescope in its warm mission phase. Among thelightcurves, 57 sources are cluster members identifiedbased on their spectral-energy distribution and X-rayemission. Almost all cluster members show significantvariability. The amplitude of the variability is larger in moreembedded YSOs. Ten out of 57 cluster members haveperiodic variations in the lightcurves with periods typicallybetween three and seven days, but even for those sources,significant variability in addition to the periodic signal canbe seen. No period is stable over 1.6 years. Non-periodiclightcurves often still show a preferred timescale ofvariability which is longer for more embedded sources.About half of all sources exhibit redder colors in a fainterstate. This is compatible with time-variable absorptiontowards the YSO. The other half becomes bluer whenfainter. These colors can only be explained with significantchanges in the structure of the inner disk. No relationbetween mid-IR variability and stellar effective temperatureor X-ray spectrum is found.Author(s): Hans Moritz Guenther (SAO)

Contributing teams: YSOVAR

419.06 – Accretion Shocks on T Tauri Stars:Plans for a Lab-Astro ExperimentWe present plans for a laboratory astrophysics experimentof a scaled accretion shock at the surface of a classical TTauri star. By creating a plasma jet (representing theaccreting material) and colliding it with a solid block(representing the surface of the T Tauri star), we hope togain insight into the structure and morphology of T Tauriaccretion shocks. Magnetic fields may play crucial role inthis phenomenon, and therefore we intend to conduct ourexperiment with imposed magnetic fields up to 8 T. Wehave a day of experiments planned on the OMEGA laser inMay 2014; some preliminary data may be available in timefor this conference. This work is funded by the U.S.Department of Energy, through the NNSA-DS and SC-OFESJoint Program in High-Energy-Density Laboratory Plasmas,grant number DE-NA0001840, and the National Laser UserFacility Program, grant number DE-NA0000850, andthrough the Laboratory for Laser Energetics, University ofRochester by the NNSA/OICF under Cooperative AgreementNo. DE-FC52-08NA28302.Author(s): Rachel Young (University of Michigan), Carolyn Kuranz(University of Michigan), R. Paul Drake (University of Michigan), DustinFroula (Laboratory for Laser Energetics), J. Ross (Lawrence LivermoreNational Laboratory), Chikang Li (Massachusetts Institute of Technology),Gennady Fiksel (Laboratory for Laser Energetics)

419.07 – Identifying New Members ofNearby Moving GroupsOur group has assembled a sample of 14,000 stars ofspectral types B9-M9 with measured UVW Galactic spacevelocities and lying within 125 pc of Earth. We haveidentified candidate members of three nearby young (lessthan 100 Myr) moving groups. For stars of spectral typesG5 and later, we have used the Kast spectrometer on theShane 3m telescope at Lick Observatory to measure lithiumabundance in order to determine stellar ages. With the datawe have obtained from this run, we will be able to establishwhether our candidates are bona fide members of themoving groups in question. I will be presenting thepreliminary results from this survey, including spectra ofthe ~50 stars observed thus far. These nearby young starswill make excellent targets for direct imaging followupsurveys, since any giant planets around young stars willstill be warm, and will therefore be bright enough to detectwith instruments like GPI.Author(s): Erika Holmbeck (UCLA), Laura Vican (UCLA)

419.08 – Characterizing Turbulence inProtoplanetary Disks: Gravito-Turbulencevs. the MRI in 3DCharacterizing turbulence in protoplanetary disks is crucialfor understanding how they accrete and spawn planets.Recent measurements of spectral line broadening promiseto diagnose turbulence, with different lines probingdifferent depths. We use 3D local hydrodynamic simulationsof cooling, self-gravitating disks to resolve how motionsdriven by “gravito-turbulence” vary with height. We findthat gravito-turbulence is practically as vigorous at altitudeas at depth. The near-uniformity of turbulent velocities isenforced by the long-range nature of gravity. By contrast,turbulence driven by the magnetorotational instability (MRI)exhibits strong height dependence. The distinct verticalprofiles of gravito-turbulence vs. MRI turbulence may beused in conjunction with measurements of non-thermallinewidths at various depths to identify the source oftransport in protoplanetary disks.Author(s): Ji-Ming Shi (University of California, Berkeley), EugeneChiang (University of California, Berkeley)

419.09 – Herschel Observations of DustyDebris DisksWe present results from several Herschel surveys of debrisdisks around nearby, young stars. The first survey was anOT-1 project based on Herschel PACS far-infraredphotometry of six stars to search for the cold component ofpreviously discovered warm debris disks. If the coldcomponent exists, then collisions between cometary bodiesin the cold belt may be feeding the grain population of thewarm dust component. If no cold component is seen, thenthe observed warm dust is likely the result of a recentcollision between planetary embryos in the terrestrialplanet zone. A second survey was an OT-2 PACS program tofurther characterize the SEDs of more than a dozen knowndebris disks. In addition to these two surveys, we presentPACS photometry of the debris disk at the star V488 Perthat extends its SED into the far-infrared. V488 Per has thelargest fractional infrared luminosity (percentage of itsbolometric luminosity) known for any main sequence star.Author(s): Laura Vican (UCLA), Joseph Rhee (California StatePolytechnic University), Ben Zuckerman (UCLA), Carl Melis (UCSD), InseokSong (University of Georgia)

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420 – Stars, Stellar Evolution and So On PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

420.01 – Application of the 2013 Wilson-Devinney Program’s Direct DistanceEstimation procedure and enhanced spotmodeling capability to eclipsing binaries instar clustersA paradigm method to calibrate a range of standardcandles by means of well-calibrated photometry ofeclipsing binaries in star clusters is the Direct DistanceEstimation (DDE) procedure, contained in the 2010 and2013 versions of the Wilson-Devinney light-curve modelingprogram. In particular, we are re-examining systemspreviously studied in our Binaries-in-Clusters program andanalyzed with earlier versions of the Wilson–Devinneyprogram. Earlier we reported on our use of the 2010version of this program, which incorporates the DDEprocedure to estimate the distance to an eclipsing systemdirectly, as a system parameter, and is thus dependent onthe data and analysis model alone. As such, the deriveddistance is accorded a standard error, independent of anyadditional assumptions or approximations that suchanalyses conventionally require. Additionally we have nowmade use of the 2013 version, which introduces temporalevolution of spots, an important improvement for systemscontaining variable active regions, as is the case for thesystems we are studying currently, namely HD 27130 in theHyades and DS And in NGC 752. Our work provides someconstraints on the effects of spot treatment on distancedetermination of active systems.Author(s): Eugene Milone (University of Calgary), Stephen Schiller(University of Calgary)

420.02 – The X-ray Binary J1118+480:Starspots and the Resumption of MassTransferWe obtained high-speed optical photometry of the blackhole X-ray binary J1118+480 on 25 nights in 2004 - 2005and 2010 - 2012. The system was in quiescence during the2004 - 2005 observations. The orbital light curve wasdominated by a two-humped ellipsoidal variation of thesecondary star. The light curve was highly stable and therewas no detectable contribution to the light curve from masstransfer and accretion processes. The orbital light curve in2004-2005 was, however, asymmetric in orbital phase,which is inconsistent with pure ellipsoidal variations. Weattribute the asymmetry to spots on the secondary star.Synthetic light curves produced by models including justellipsoidal variations and a single large spot on the surfaceof the secondary star fit the observed light curve well.J1118+480 was up to 20% brighter in 2010-2012 and itslight curve displayed rapid flickering, indicating that masstransfer had resumed by then.Author(s): Isaac Lopez (Univ. of Texas at El Paso), Paul Mason (Univ.of Texas at El Paso), Edward Robinson (Univ. of Texas at Austin), RobertHynes (Louisiana State Univ.)

420.03 – Analysis of the Short period SolarType binary, V1073 Herculis and thedetection of a possible brown dwarfcompanionV1073 Herculis is a very short period, P= 0.294281673(4)day eclipsing binary. It was observed on May 7, 9, 11, and12, 2012 by at the Lowell Observatory 31” NURO reflectorby Samec, Benkendorf and Dignan. The analysis wascarried out by Kring, Samec and Shebs. The period studyconsisting of some 54 times of minimum light included fournew timings determined through this study: JD Hel Min I =2456056.8549±0.0002, 2456058.7685±0.0002,2456058.91485±0.00008, 2456059.9455±0.0001. Theyreveal a very low amplitude, <0.003 d sinusoidal variationand a period of 11.25 years, which may indicate thepresence of a Brown Dwarf third component and the firstdetection of such a body through an O-C study. 2MASSphotometry reveals that the temperature of the binary is~5200K. The Wilson-Devinney Program preliminary solutionreveals that the system has a mass ratio of 0.4, nearlyidentical component temperatures and a cool magneticspot with a T-factor of 0.88 with a spot radius of 23degrees. The Roche Lobe fill-out is 0.18. The inclination isnearly 80 degrees. We wish to think NURO for its allocationof observing time.Author(s): Travis Shebs (Bob Jones University ), James Kring (BobJones University ), Ronald Samec (Bob Jones University )

420.04 – On the Spectroscopic Properties ofthe Retired A Star HD 185351Doppler-based planet surveys have shown that, besidesmetallicity, the planet occurrence is also correlated withstellar mass, increasing from M to F-A spectral types.However, it has recently been argued that the subgiants(which represent A stars after they evolve off the mainsequence) may not be as massive as suggested initially,which would significantly change the correlation found. Tostart investigating this claim, we have studied the subgiantstar HD 185351, which has precisely measured physicalproperties based on asteroseismology and interferometry.An independent spectroscopic differential analysis based onexcitation and ionization balance of iron lines yielded theatmospheric parameters Teff = 5035 ± 29 K, log g = 3.30 ±0.08 and [Fe/H] = 0.10 ± 0.04. These were used inconjunction with the PARSEC stellar evolutionary tracks toinfer a mass M = 1.77 ± 0.04 M?, which agrees well withthe previous estimates. Lithium abundance was alsoestimated from spectral synthesis (A(Li) = 0.93 ± 0.30)and, together with Teff and [Fe/H], allowed to determine amass M = 2.0 [+0.1 -0.3] M?, which is independent of thestar's parallax and surface gravity. Although a variation ofup to ~0.4 M? can be observed between the different massestimates, all values are higher than 1.6 M?, whichsupports the correlation between planet occurrence andstellar masses.Author(s): Luan Ghezzi (Harvard-Smithsonian Center forAstrophysics), José-Dias Do Nascimento (DFTE/Universidade Federal doRio Grande do Norte), John Johnson (Harvard-Smithsonian Center forAstrophysics)

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420.05 – Testing Stellar Models withAccurate Parallaxes and Abundances ofMetal-Poor StarsAn abundance analysis of nine low metallicity mainsequence stars using high dispersion spectroscopy from theKeck/HiRES and Magellan/Mike spectrographs is presented.These stars have recently had their parallaxes determinedusing the Fine Guidance Sensors on HST. Currently, the vanLeeuwen (2007) Hipparcos catalog contains only one starwith [Fe/H] <-1.4 suitable for use in main sequence fitting;the results of this work, along with the HST parallaxmeasurements, will increase the number of stars availablefor main sequence fitting by an order of magnitude.Preliminary [Fe/H] and [?/Fe] abundances have beenobtained. Eight of the nine target stars have metallicity[Fe/H] < -1.5 that can be used in the development ofaccurate stellar models for low metallicity stars. Theseresults extend the range of stellar metallicities that can bemodeled and will help to improve the accuracy of distancedeterminations to metal-poor GCs.Author(s): Erin O'Malley (Dartmouth College), Andrew McWilliam(The Observatories of the Carnegie Institute of Washington), BrianChaboyer (Dartmouth College)

420.06 – Photometry on Metal-Poor Starswith HST ParallaxesStellar evolution models and isochrones of metal-poor starsare widely used in astrophysics. However, there are fewobservational tests of the validity of these models belowmetallicities of [Fe/H] = -1.5. To remedy this situation, HSThas determined parallaxes for 9 metal-poor main sequencestars. Here, we present new ground-based photometry ofthese stars. The observations were obtained at MDMobservatory in March of 2012 over the course of five nights.Our photometry is compared to literature values andcombined with parallax results to obtain absolutemagnitudes for these stars. The locations of the stars on acolor-magnitude diagram are compared to theoreticalmodels.Author(s): Meridith Joyce (Dartmouth College), Brian Chaboyer(Dartmouth College), Gregory Feiden (Dartmouth College), MorganMatthews (Dartmouth College), G. Benedict (McDonald Observatory),Barbara McArthur (McDonald Observatory), Thomas Harrison (New MexicoState University), Andrew McWilliam (Carnegie Institute of Washington),Edmund Nelan (Space Telescope Science Institute), Richard Patterson(University of Virginia), Ata Sarajedini (University of Florida)

420.07 – Numerical Simulations ofMicroturbulence in Hot Stellar AtmosphersMicroturbulence is one of the factors that determines thewidth of a spectral line in stellar atmospheres along withDoppler broadening and other forms. At this point in time ithas been used as a parameter to match the observationalresults without explanation of why the microturbulencevalue is what it is. Here we are modeling hot stellaratmospheres with a 3D radiative hydrodynamic code todetermine the causes and scale of microturbulent motionsand their contributions to non-LTE scattering in resonanceline transfer.Author(s): Michelle Deady (University of Toledo), LawrenceAnderson-Huang (University of Toledo)

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421 – Stars: Variable and Explosive PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

421.01 – Probing rotational dynamoextremes: X-ray and optical spectroscopy ofthe 0.5 day period eclipsing binary, HD79826.The highly modulated optical light curve of HD 79826(spectral type G5) was discovered in the Chandraguide-star light curves, indicating a period of about 0.5days, a strong and migrating distortion wave, and a shalloweclipse. We subsequently obtained simultaneous Chandrahigh resolution X-ray spectra and optical photometry, alongwith contemporaneous ground-based photometry andspectra. X-ray rotational or eclipse modulation was totallyobscured by X-ray variability and flares. X-ray spectra arecharacterized by coronal emission near the saturation limitof Lx/Lbol = 0.001. Optical spectra show extremelyrotationally broadened features, variable with orbital phase.Optical light curves show the modulation to be not onlyrapidly migrating in phase, but also of variable amplitude.We will further characterize the X-ray emission throughmeasurements of line widths, velocities, and fluxes, andprovide coronal plasma models. This star is near or at thelimits of dynamo saturation, and since it is partiallyeclipsing, has potential to be well characterized in terms offundamental stellar parameters. Acknowledgments: Thiswork was supported by NASA through the SmithsonianAstrophysical Observatory (SAO) contract SV3-73016 forthe Chandra X-Ray Center and Science Instruments.Author(s): David Huenemoerder (MIT Kavli Institute), Joy Nichols(CfA), David DePalma (CfA), David Garcia-Alvarez (IAC), Norbert Schulz(MIT Kavli Institute), Claude Canizares (MIT Kavli Institute)

421.02 – Variable Star Discoveries forResearch Education at the Phillips AcademyObservatoryThe discovery and publication of unknown variable stars byhigh school students is a highly engaging activity in a newhands-on research course developed at Phillips Academy inAndover, Massachusetts. Students use MPO Canopussoftware to recognize candidate variable stars in imageseries typically recorded for asteroid rotation studies.Follow-up observations are made using the 16-inch DFMtelescopes at the Phillips Academy Observatory and at theHUT Observatory near Eagle, Colorado, as well as with aremote-access 20-inch at New Mexico Skies Observatorynear Mayhill, New Mexico. The Catalina Sky Survey canprovide additional photometric measurements. Confirmedvariables, with light curves and periods, are submitted tothe International Variable Star Index and Journal of theAmerican Association of Variable Star Observers. Asteroidrotation studies are published in Minor Planet Bulletin.Author(s): Caroline Odden (Phillips Academy), Seokjun Yoon (PhillipsAcademy), Emily Zhu (Phillips Academy), John Little (Phillips Academy),Isabel Taylor (Phillips Academy), Ji Seok Kim (Phillips Academy), JohnBriggs (HUT)

421.03 – The RR Lyrae Period-LuminosityRelation in IRAC Channels 1 and 2We present new period-luminosity relations for RR Lyraevariables in the globular cluster ? Centauri derived fromtime-resolved IRAC data, the slopes of which are inreasonable agreement with those derived from WISE databy Madore et al (2013), Klein et al (2014), and Dambis et al(2014). We also present an investigation into thecorrelation of the PL residuals with individual metallicitiesfrom Rey et al (2000) and Sollima et al (2006). We find nocompelling evidence for a metallicity correlation in theresiduals, based on a spread of up to 1.19 dex in [Fe/H].Author(s): Meredith Durbin (Pomona college), Victoria Scowcroft(Carnegie Observatories), Wendy Freedman (Carnegie Observatories),Barry Madore (Carnegie Observatories), Andrew Monson (CarnegieObservatories), Mark Seibert (Carnegie Observatories), Jeffrey Rich(Carnegie Observatories)

421.04 – Swift/BAT detection of hard X-raysfrom Tycho;s Supernova Remnant: Evidencefor 44TiWe report Swift/BAT survey observations of the Tychosupernova remnant, performed over a period of 104 month.A total exposure of 19.6 Ms was used to detect significanthard X-ray emission up to about 100 keV. Excess emissionabove this continuum in the 60-85 keV band was found,consistent with line emission from radioactive 44T. Wediscuss the implications of these results in the context ofthe galactic supernova rate, and nucleosynthesis in Type IIand Type Ia supernova, with emphasis on the production of44Ti.Author(s): Dieter Hartmann (Clemson Univ.), Eleonora Troja (ClemsonUniv.), Wayne Baumgartner (Clemson Univ.), Craig Markwardt (ClemsonUniv.), Scott Barthelmy (Clemson Univ.), Neil Gehrels (Clemson Univ.),Alberto Segreto (Clemson Univ.), Valentina La Parola (Clemson Univ.)

Contributing teams: Swift/BAT

421.05 – Light Curves of Type IILSupernovaeThe absolute-magnitude light curves of 17 Type IILsupernovae are studied. A light curve model is used in theanalysis. From the model, we are able to make estimates ofthe progenitor radius, the kinetic energy in the explosion,the total ejected mass and nickel mass in the explosion aswell as the rise time for each supernova.Author(s): Dean Richardson (Xavier University of Louisiana), AaronBenner (Shippensburg University), Zachary Babyak (Purdue University),Benjamin Moore (Xavier University of Louisiana)

421.06 – Multi-Wavelength Light Curve ofSN 2014GSN 2014G received an initial spectral classification of TypeIIn (CBET 3787) as a blue continuum with some sharpemission. Later spectra (ATEL 5935) showed that it is morelikely it is a Type II-L. We present multi-band photometry forthis object from the peak until approximately 100 daysafter.Author(s): John Martin (U of Illinois Springfield), Alberto Betzler(Universidade Federal do Reconcavo da Bahia), Douglas Barrett (), AndyCason (), Tõnis Eenmäe (Tartu Observatory), Raymond Kneip (),Massimiliano Martignoni ()

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421.07 – An XMM-Newton Observation ofthe Spitzer-Detected Galactic SupernovaRemnant Kesteven 69 (G21.8-0.6)The Galactic supernova remnant (SNR) Kesteven 69(G21.8-0.6) has been the subject of intensive study acrossa broad range of the electromagnetic spectrum (from X-raythrough radio). These observations have revealed a sourcewith a radio-luminous southern rim that is interactingdramatically with an adjacent molecular cloud, as indicatedby the detection of masers toward this SNR as well as theidentification by Spitzer of a prominent infrared counterpartto the radio luminous rim. To date, the X-ray properties ofKesteven 69 remain poorly explored: while hard X-raysources seen toward this SNR have been classified as fastejecta fragments, little study has been devoted to thediffuse X-ray emission. We present a spatially-resolvedspectral analysis of this SNR where we consider both theglobal X-ray spectrum of the diffuse emission as well as thespectra of individual regions of the emission. We search forspatial variations in the temperature, ionization timescaleand elemental abundances of the plasma and compare theX-ray properties of Kesteven 69 to other Galactic SNRsknown to be interacting with adjacent molecular clouds.Initial results will be presented and discussed.Author(s): Thomas Pannuti (Morehead State University)

421.08 – A Reverse Shock in GRB 130427AWe present extensive radio and millimeter observations ofthe unusually bright GRB 130427A at z=0.340, spanning0.67 to 12 days after the burst. Taken in conjunction withdetailed multi-band UV, optical, NIR, and X-ray observationswe find that the broad-band afterglow emission iscomposed of distinct reverse shock and forward shockcontributions. The reverse shock emission dominates in theradio/millimeter and at <0.1 days in the UV/optical/NIR,while the forward shock emission dominates in the X-raysand at >0.1 days in the UV/optical/NIR. We further find thatthe optical and X-ray data require a Wind circumburstenvironment, pointing to a massive star progenitor. Usingthe combined forward and reverse shock emission we findthat the parameters of the burst are an isotropic kineticenergy of E_Kiso~2e53 erg, a mass loss rate of Mdot~3e-8Msun/yr (for a wind velocity of 1,000 km/s), and a Lorentzfactor at the deceleration time of Gamma(200s)~130. Dueto the low density and large isotropic energy, the absenceof a jet break to ~15 days places only a weak constraint onthe opening angle of theta_j>2.5 deg, and therefore a totalenergy of E_gamma+E_K>1.2e51 erg, similar to otherGRBs. The reverse shock emission is detectable in thisburst due to the low circumburst density, which leads to aslow cooling shock. We speculate that this is a requiredproperty for the detectability of reverse shocks in the radioand millimeter bands. Following on GRB 130427A as abenchmark event, observations of future GRBs with theexquisite sensitivity of VLA and ALMA, coupled withdetailed modeling of the reverse and forward shockcontributions will test this hypothesis.Author(s): Tanmoy Laskar (Harvard University), Edo Berger (HarvardUniversity), B. Zauderer (Harvard-Smithsonian CfA), Raffaella Margutti(Harvard-Smithsonian CfA), Alicia Soderberg (Harvard University), RagnhildLunnan (Harvard University), Ryan Chornock (Harvard-Smithsonian CfA)

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422 – The Sun and The Solar System PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

422.01 – An Explanation of the DifferencesBetween the Sunspot Area Scales of theRoyal Greenwich and Mt. WilsonObservatories, and the SOON Program.Several studies have shown that the sunspot areasrecorded by the Royal Greenwich Observatory (RGO)between 1874 - 1976 are about 40-50 percent larger thanthose measured by the NOAA/USAF Solar Observing OpticalNetwork(SOON) since 1966. We show here that, while thetwo measurement sets provide consistent total areas forlarge spots, the impossibility of recording small spots asanything except dots in the SOON drawings leads to anunderestimate of of small spot areas. These are moreaccurately recorded by the RGO and other programs thatuse photographic or CCD images. The large number of suchsmall spots is often overlooked. A similar explanation holdsfor the RGO umbral areas, which amount to 40 percentmore than those measured from Mt. Wilson data between1923 and 1982. The neglected small spots have a muchlower photometric contrast. Our explanation suggests,therefore, that the adjustment to spot irradiance blockingat the 1976 transition from RGO to SOON areas is smallerthan the almost 50 percent correction advanced by somerecent, purely statistical, studies.Author(s): Peter Foukal (Heliophysics, Inc.)

422.02 – Calculated Sunspot and Quiet-SunMg II Profiles Compared With IRIS DataEugene Avrett and Hui Tian Harvard-Smithsonian Center for Astrophysics 60Garden Street, Cambridge, MA 02138A new sunpsot model has been derived, consistent with theSUMER atlas data of Curdt, et al. and Mg II profile data fromIRIS. Comparisons are made with Quiet-Sun results fromboth sources. It is necessary to include molecules in thesunspot model not only account for the low brightnesstemperatures near 1850 /AA but also for the densityvariations higher in the atmosphere. The minimumtemperature is roughly 2500 K in the sunspot model and4500 K for the quiet Sun. The Mg II H line profile is centrallyreversed in both cases, with the peak intensity originatingwhere the temperature rises abruptly from the minimumvalue. The line center is formed at the top of thechromosphere where the temperature rises abruptly from10,000 K into the chromosphere-corona transition region.The calculated Mg II line center intensity is much smallerthan observed, for models constrained by the EUVcontinuum data.Author(s): Eugene Avrett (Harvard-Smithsonian CfA)

422.03 – Coronal Diagnostics from CometaryEmissionThe extreme ultraviolet (EUV) emission observed fromsungrazing comets as they pass through the solaratmosphere can be used to infer the properties of thecorona. In this paper we will discuss several of theseproperties that can be estimated from the EUVobservations of Comet Lovejoy from AIA/SDO andSWAP/PROBA2. The longevity of the emission allows us toconstrain the coronal electron density through which thecomet passes. We will also discuss how dispersion of theemitting cometary material we can be used to estimate thelocal Alfven speed in the corona. Finally, measuring thedeformation of the magnetic field as it is impacted by thecomet can be used to estimate the magnetic field strengthin this location. In the absence of the comet, none of theseparameters are directly measurable in the corona.Sungrazing comets are thus unique probes of the solaratmosphere.Author(s): Paul Bryans (NASA Goddard Space Flight Center),William Pesnell (NASA Goddard Space Flight Center), Daniel Seaton (RoyalObservatory of Belgium), Matthew West (Royal Observatory of Belgium)

422.04 – Spectropolarimetric Observationsof a Small Active Region with IBISWe have used the Interferometric BI--dimensionalSpectrograph (IBIS) instrument at the Dunn Solar Telescopeto measure the polarimetric Stokes IQUV signals for thesmall active region, NOAA 11304. We used three linesgenerally corresponding to three atmospheric heightsranging from the photosphere to low corona: Fe I 6302?,NaI 5896?, and CaII 8542?. Each set of profiles has beeninverted using the NICOLE code to determine the vectormagnetic field at the three heights throughout the field ofview, or the line--of--sight field, as allowed by the level ofpolarization signal. Comparisons are made between themagnetic and thermal structures with the goal ofconstraining chromospheric models with the informationobtained at multiple heights.Author(s): Lucas Tarr (Montana State University), Philip Judge(NCAR/HAO)

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422.05 – The Quasi-Annual Forcing of TheSun’s Eruptive, Radiative, and ParticulateOutputThe eruptive, radiative, and particulate output of the Sunare modulated by our star’s enigmatic 11-year sunspotcycle. Over the past year we have identified observationalsignatures which illustrate the ebb and flow of the 11-yearcycle – arising from the temporal overlap of migratingactivity bands which belong to the 22-year magneticactivity cycle. (At the 2012 Fall AGU Meeting, Leamon &McIntosh presented a prediction of minimum conditionsdeveloping in 2017 and Cycle 25 sunspots first appearing inlate 2019.) As a consequence of this work we have deducedthat the latitudinal interaction of the oppositely signedmagnetic activity bands in each hemisphere (and acrossthe equator near solar minimum) dramatically impacts theproduction of Space Weather events such as flares andCoronal Mass Ejections (CMEs). The same set ofobservations also permits us to identify a quasi-annualvariability in the rotating convecting system which resultsin a significant local modulation of solar surfacemagnetism. That modulation, in turn, forces prolongedperiods of significantly increased flare and CME production,as well as significant changes in the Sun's ultraviolet (UV),extreme ultraviolet (EUV), and X-Ray irradiance.Author(s): Robert Leamon (Montana State University), ScottMcIntosh (HAO/NCAR)

Contributing teams: The Whomps Team

422.06 – Off Limb Solar Adaptive OpticsLong-exposure spectroscopy and spectro-polarimetry atnear-infrared wavelengths is one of the preferred toolsdeployed to measure the physical properties ofprominences, including the prominence magnetic field.However, until now, it was not possible to observeprominences in sufficient detail to allow us to understandtheir dynamical properties. In order to understand solarprominences, we need to observe them at sub-arcsecondspatial resolution, with a temporal cadence sufficient tomake highly transient structures visible. Adaptive opticscapable of locking-on to off-limb prominence structure hasbeen proven successful. It has been shown to allow fordiffraction limited spectroscopy and polarimetry ofprominence structure. This adaptive optics system willallow scientists to come one step closer to understandingthe true nature of solar prominences.Author(s): Gregory Taylor (New Mexico State University)

422.07 – Modeling of SDO/HMI spectro-polarimetric data and center-to-limbvariation effects with 3D MHD simulationsObservations with the Solar Dynamics Observatory (SDO),and, in particular, Helioseismic and Magnetic Imager (HMI)provide a unique opportunity to investigate variousphenomena simultaneously over the whole solar disk.Current state-of-the-art numerical simulations allow us tomodel the observational data with a high degree of realism,and use the artificial data for interpretation of observedproperties ("observables") in terms of the physicalconditions, for the testing of new data analysis techniquesand the improvement of data calibration. In the currentstudy we use realistic-type 3D radiative MHD simulations ofthe upper turbulent convective layer and atmosphere of theSun, obtained with the SolarBox code, and employ thespectro-polarimetric radiative transfer code SPINOR toconvert the simulated data into Stokes profiles of the HMIFe I 6173 A line for different conditions in the solaratmosphere. For testing the HMI calibration the syntheticStokes profiles are processed through the SDO/JSOCsimplified data analysis pipeline. We investigate propertiesof the HMI observables for various solar features, variationsof the line formation height for different angular distancesfrom the disk center, effects of the spatial resolution andiron abundance, and pay particular attention to the center-to-limb variations effects playing important role in localhelioseismology measurements.Author(s): Irina Kitiashvili (Stanford University), Sebastien Couvidat(Stanford University)

422.08 – Limits of Astrometric andPhotometric Precision on KBOs using SmallTelescopesWe conducted photometric and astrometric measurementson Haumea and Makemake, two Kuiper Belt Objects whichare typically observed by 1-meter class telescopes orlarger, with the goal of testing the limitations of smalltelescopes. Here we present our measurements of Haumeaand Makemake obtained between June 5th, 2013 and July31st, 2013 with the 14-inch Wallace AstrophysicalObservatory (WAO) telescopes. Using photometry, wedetermined that Haumea and Makemake have R-bandmagnitudes of 17.225±0.347 and 16.850±0.107respectively. These values agree with the previous R-bandmeasurements of 17.240±0.030 (Lacerda et al. 2008) and16.802±0.041 (Rabinowitz et al. 2007) for Haumea andMakemake respectively. We obtained rotational light curvesfor Haumea and Makemake over eight separate nights,again by analysing the photometry observations.Astrometry yielded residuals of -0.039±0.025 arcseconds inRA and 0.234±0.017 arcseconds in DEC for Makemake, and0.295±0.077 arcseconds in RA and 0.184±0.0554arcseconds in DEC for Haumea. These results, whensubmitted to the minor planet center, are able to increasethe accuracy of the JPL ephemeris. Additionally, wecalculated that observing Haumea with two 14-inchtelescopes and Makemake with four 14-inch telescopes, inideal conditions, could resolve their periodicity. Weconclude that with improved observing techniques andmodern CCD cameras, it is possible to utilize smalltelescopes in universities around the world to observe largeKBOs and obtain accurate photometric and astrometricresults.Author(s): Evangelia Anna Markatou (MIT), Amanda Wang (MIT),Molly Kosiarek (MIT), Emilie Dunham (Case Western Reserve University)

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423 – Topics in Cosmology PostersPoster Session – Essex Ballroom and America Foyer – 05 Jun 2014 09:00 AM to 02:00 PM

423.01 – The Effective Field Theory of DarkMatter and Structure FormationWe develop the effective field theory of cosmological largescale structure. We start from the collisionless Boltzmannequation and integrate out short modes of a darkmatter/dark energy dominated universe (LambdaCDM)whose matter is comprised of massive particles as used incosmological simulations. This establishes a long distanceeffective fluid, valid for length scales larger than thenon-linear scale ~ 10 Mpc, and provides the completedescription of large scale structure formation. Extractingthe time dependence, we derive recursion relations thatencode the perturbative solution. This is exact for thematter dominated era and quite accurate in LambdaCDMalso. The effective fluid is characterized by physicalparameters, including sound speed and viscosity. These twofluid parameters play a degenerate role with each otherand lead to a relative correction from standard perturbationtheory of the form ~ 10^{-6}c^2k^2/H^2. Starting fromthe linear theory, we calculate corrections to cosmologicalobservables, such as the baryon-acoustic-oscillation peak,which we compute semi-analytically at one-loop order. Dueto the non-zero fluid parameters, the predictions of theeffective field theory agree with observation much moreaccurately than standard perturbation theory and weexplain why. We also discuss corrections from treating darkmatter as interacting or wave-like and other issues.Author(s): Mark Hertzberg (MIT)

423.02 – Cosmic Metallicity fromZnII-Selected QSO Absorption Line Systemsnear Redshift z=1.2We present metallicity results for a sample of dampedLyman-alpha (DLA) quasar absorption line systems selectedfor strong ZnII absorption at redshift z ? 1.2. DLA systemstrack cosmologically intervening neutral gas regions thatfall along the sightlines to background quasars. The samplewas compiled from the University of Pittsburgh catalog ofstrong, intervening MgII systems observed in SDSS quasarspectra. We selected candidates by examining the spectralregions where weak, unsaturated metal lines (such as ZnIIand CrII) for such systems were predicted to exist, with theaim of finding a representative sample of the strongestmetal-line column density DLA systems in the universe.Follow-up HST-STIS G230L UV spectroscopy of the samplesystems was obtained to measure their Lyman-alphaabsorption profiles and derive their HI column densities.Since Zn is not depleted onto grains and exists primarily inthe singly ionized state, measurement of N(HI) coupled withequivalent width measurements of ZnII lines allows a directmeasurement of the metal abundance in such systems.Strong ZnII absorption may be due to either large columns

(e.g., N(HI) ~3x1021 atoms cm-2) of typicallylow-metallicity DLA gas, or weaker columns (e.g., N(HI)~

2x1020 atoms cm-2) of higher metallicity gas. Our sample,therefore, can test the upper envelope of the distribution ofneutral-gas-phase metallicities near redshift z=1.2.Sincethese DLAs are selected on the basis of their extrememetal-line properties, analysis of their metallicities anddust-to-gas ratios can constrain the range of propertiesexhibited by DLA systems.Author(s): Eric Monier (SUNY College at Brockport), David Turnshek(University of Pittsburgh), Sandhya Rao (University of Pittsburgh), GendithSardane (University of Pittsburgh), Daniel Burdette (SUNY College atBrockport)

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423.03 – How Do Galaxy Pairs Populate theDark Matter Haloes?We Analyze the clustering of photometrically selectedgalaxy pairs by using the halo-occupation distribution(HOD) statistics. We measure the two-point auto-correlationfunctions, \omega_(\theta), for galaxies and galaxy pairsand find their HODs to model the clustering. Our results aresuccessfully fit by the HOD models and we can see theseparation of '1-halo' and '2-halo' clustering terms for bothsingle galaxies and galaxy pairs. We find that the galaxypairs generally have larger clustering amplitudes thansingle galaxies, and the quantities after the HOD fitting, i.e.effective mass M_{eff} and linear bias b_g, are also largerin pairs. We find the central fractions for galaxy pairs aresignificantly higher than that of the single galaxies, whichconfirms that the galaxy pairs are formed at the center ofmore massive haloes. We also fit HOD models to thecorrelation functions so that we can quantify thedifferences for i) early-early and late-late type galaxy pairsand find the former type one shows stronger clusteringsignals and have larger bias than the latter one; ii)high-flux-contrast and low-flux-contrast galaxy pairs andfind the former has stronger clustering structures; and iii)bright and dim samples for galaxies and galaxy pairs andfind the bright samples are stronger clustered than the dim

samples.Author(s): Yiran Wang (University of Illinois at Urbana-Champaign), Robert Brunner (University of Illinois at Urbana-Champaign)

423.04 – Intrinsic Alignments of galaxies inSDSS-III BOSS LOWZ sample.Intrinsic Alignments (IA) of galaxies, i.e. correlations ofgalaxy shapes with each other (II) or with the density field(gI), are one of the major astrophysical source ofcontamination for weak lensing surveys (Hirata & Seljak2004, Mandelbaum+ 2006, Hirata+ 2007, Joachimi+ 2011).We will present the results of IA measurements of galaxies(II and gI) using the SDSS-III BOSS LOWZ sample, in redshiftrange 0.16<z<0.36. Taking advantage of the size andluminosity range of LOWZ sample we have extended the IAmeasurements for spectroscopic LRGs to more typical lowerluminosity galaxies. We also study the environmentdependence of IA by splitting the sample into field andgroup galaxies, which are further split into satellite andcentral galaxies. We show that group galaxies have muchstronger IA at small scales, while central and field galaxieshave similar IA at large scales.Author(s): Sukhdeep Singh (McWilliams center for Cosmology,Carnegie Mellon University), Rachel Mandelbaum (McWilliams centerfor Cosmology, Carnegie Mellon University)

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401 – Gamma-ray Constraints on the EBL and the IGMF IMeeting-in-a-Meeting – America Ballroom North/Central – 05 Jun 2014 10:00 AM to 11:30 AM

The light emitted by stars throughout the history of the Universe is encoded in the intensity of the extragalacticbackground light (EBL). Characterization of the EBL and its evolution provides insight into the nature of starformation and galaxy evolution. Direct measurements of the EBL are difficult due to local intense foregroundssuch as the zodiacal light and emission from our own Galaxy. Gamma-ray astronomy provides a valuable indirectprobe of the EBL since high-energy gamma rays may interact with photons of the EBL and generate positron-electron pairs. This introduces an attenuation feature in the spectra of distant gamma-ray sources that can beused to place sensitive constraints on the opacity of the universe to gamma-rays and on the energy density of theEBL. Moreover, the electron-positron pairs can generate an electro-magnetic cascade that reprocessed the initialphoton energy to lower gamma-ray energies producing spectral, spatial and temporal signatures that can be usedto place sensitive constraints on the strength of the intergalactic magnetic field (IGMF). Recent studies usinggamma-ray blazars claimed the detection of EBL-induced absorption signatures consistent with the minimumlevel of EBL intensity expected given the established star formation rate. Thus, there is little room for anadditional, truly diffuse component generated at much higher redshifts. At the same time, other studies based ongamma-ray blazars constrained the strength of the IGMF to be >1e-17 Gauss (depending on the coherent lengthand source activity timescale). Our proposed meeting-in-meeting will focus on up-to-date results and currentlyon-going projects to constrain the strength of the IGMF and further characterize the EBL intensity, its evolution,and its impact on on our understanding of star formation. The first session will cover topics related to the EBL, andits constraints while the second one will deal with the cascade formation, composition and propagation in theintergalactic medium and the derived constraints on the strength of the IGMF.

Chair(s):Justin Finke (US Naval Research Laboratory)

Organizer(s):Marco Ajello (Berkeley)

401.01 – The Extragalactic BackgroundLight and the Gamma-Ray Opacity of theUniverseThe Extragalactic Background Light (EBL) is one of thefundamental observational quantities in cosmology. Allenergy releases from resolved and unresolved extragalacticsources, and the light from any truly diffuse background,excluding the cosmic microwave background (CMB),contribute to its intensity and spectral energy distribution.It therefore plays a crucial role in cosmological tests for theformation and evolution of stellar objects and galaxies, andfor setting limits on exotic energy releases in the universe.The EBL also plays an important role in the propagation ofvery high energy gamma-rays which are attenuated enroute to Earth by pair producing gamma-gammainteractions with the EBL and CMB, affecting the GeV-TeVspectrum of blazars. Knowledge of the EBL intensity andspectrum will therefore allow the determination of theintrinsic blazar spectrum, and conversely, knowledge of theintrinsic gamma-ray spectrum will set strong limits on theEBL and its evolution. In this talk I will review the latestdevelopments in the determination of the EBL and its effecton the gamma-ray opacity of the universe.Author(s): Eli Dwek (NASA's GSFC)

401.02 – The Gamma-Ray Opacity of theUniverse & Indirect Measurements of theEBLAs gamma rays with energies of 20 GeV to 10s of TeV travelover extragalactic distances, their energy-dependent crosssection with diffuse photons from the EBL (ExtragalacticBackground Light) results in electron-positron pairproduction. Thereby, absorption by the EBL affects theenergy spectra of all extragalactic gamma-ray sources,effectively creating an energy dependent gamma-rayhorizon. Observations of blazars with current generationsatellite- and ground-based telescopes have revealed lowgamma-ray opacities, much lower than previouslyexpected. In turn, the energy spectra of blazars at GeV toTeV energies now also provide strong constraints to the EBLin the UV/optical light, the near-IR and the mid-IR. Whilephotons with energies of 1 TeV or larger photons should notreach the observer from a redshift of z ~ 1 or larger, theproduction of secondary photons via hypothesized newphysics (Axion-Like Particles), or cosmic-ray inducedcascades could render high-redshift sources observable atTeV energies. Therefore, measurements of the gamma-rayopacity of the universe are also relevant for testingpropagation models that are build on physical scenariosbeyond gamma-ray absorption via pair production. Acompletely self-consistent picture, where directmeasurements of the EBL or lower limits from galaxycounts, converge with indirect measurements with gammarays is yet to be achieved with observations. Recent resultsfrom gamma-ray observations, their interpretation andcaveats will be discussed.Author(s): Frank Krennrich (Iowa State University)

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401.03 – Gamma-ray Cosmology in thePre-CTA EraGamma-ray astronomy at TeV energies has beenenvisioned as a powerful tool to probe the extragalacticbackground light (EBL) since the early '60s, three decadesbefore the first extragalactic TeV sources were evendetected. Gamma rays can indeed interact along the line ofsight with the EBL, creating electron-positron pairs. Thisresults in an energy- and redshift-dependent absorption ofthe emitted spectra which, when detected, would conveyinformation on the broad-band density of the EBL and on itsevolution across the billion-years journey of the gammarays. The coarse structure of the energy dependence of theabsorption, that softens the gamma-ray spectrum, hasbeen used in the '90s and '00s to set indirect upper limitson the EBL density. The main limitation arose fromaccounting for the intrinsic spectral softening, related tothe radiative processes and acceleration mechanisms atplay in the emitters. The beginning of the '10s has seen theovercoming of this limitation, yielding the first indirectmeasurements of the EBL absorption by H.E.S.S, belowz<0.2, and by Fermi-LAT, mostly above z>0.5. In this talk, Iwill discuss the method employed by H.E.S.S. andFermi-LAT to detect the EBL absorption, by means of ascaling of the EBL density, and compare their results withdirect limits in the UV, optical and near-infrared bands. I willpropose an extension of this method to constrain thespectrum and evolution of the EBL, and/or to search for

anomalies in gamma-ray spectra. An abnormal level ofabsorption could probe a large panel of physical processes,be they cosmic-ray acceleration and reprocessing along theline of sight, or physics beyond the standard model such asLorentz invariance violation or photo-axion conversion. Thegolden age of gamma-ray cosmology is yet to come duringthe next decade, with the upgrade of current-generationinstruments and the upcoming Cherenkov Telescope Array,CTA.Author(s): Jonathan Biteau (SCIPP / UCSC)

401.04 – The Gamma-ray Opacity of theUniverse up to redshift 3The extragalactic background light (EBL) leaves a distinctimprint on the gamma-ray spectra of distant sources thatcan be used to constrain its intensity. The data collected bythe Fermi Large Area Telescope (LAT) have already allowedus to constrain the EBL intensity up to redshift 1.6. In thistalk we will report on a new measurement, usingflat-spectrum radio quasars, of the EBL attenuation up toredshift 3. We will discuss how this new measurement,together with previous ones at different gamma-rayenergies, can be used to constrain the evolution of the EBLintensity.Author(s): Marco Ajello (Clemson University), Anita Reimer(Innsbruck University), Luis Reyes (California Polythenic State University),Alberto Dominguez (University of California Riverside), Sara Buson (IstitutoNazionale di Fisica Nucleare)

Contributing teams: Fermi-LAT team

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402 – Solar Wind and Heliospheric ConnectionsMeeting-in-a-Meeting – America Ballroom South – 05 Jun 2014 10:00 AM to 11:30 AMChair(s):Mari Paz Miralles (Harvard-Smithsonian CfA)

402.01 – Coronal Density StructureRevealed by Comet Lovejoy (C/2011 W3)Images of Comet Lovejoy (C/2011 W3) obtained with AIAare dominated by emission from moderately ionized oxygen(O III - O VI). The images show striations due to magneticfield structure. In each striation, the oxygen emissionmoves along the magnetic field and stretches with time.The speed and the rate of broadening are related to theparallel and perpendicular components of the velocities ofthe cometary neutrals when they become ionized andbehave as pickup ions. The intensity structure indicatesdensity contrasts of a factor of 6 between neighboringmagnetic flux tubes on scales of around 4000 km. Thatimplies substantial variation in Alfven speeds, which resultsin dispersion and dissipation of Alfven waves. Thisobservation imposes an upper limit in the outer scale of theturbulence spectrum in the corona and suggests thatdensity structures may affect the heating of the corona andthe driving of the solar wind.Author(s): John Raymond (Harvard-Smithsonian, CfA), PatrickMcCauley (Harvard-Smithsonian, CfA), Steven Cranmer (Harvard-Smithsonian, CfA), Cooper Downs (Predictive Sciences, INC)

402.02 – Periodic Density Structures andthe Source of the Slow Solar WindPeriodic density structures with length-scales of hundredsto several thousands of megameters, and frequencies oftens to hundreds of minutes, are observed regularly in thesolar wind at 1 AU. These structures coexist with, but arenot due to, fluctuations in the plasma resulting from theturbulent cascade. Two lines of evidence suggest thatperiodic density structures are formed in the solar coronaas part of the slow solar wind release and/or accelerationprocesses. The first is the identification of correspondingchanges in compositional data in situ, and the other is theidentification of periodic density structures in the innerHeliospheric Imaging data onboard the STEREO/SECCHIsuite. In this presentation, we show the results of trackingperiodic structures identified in the SECCHI/Hi1 imagesdown through the corresponding SECCHI/Cor2 images. Wedemonstrate that the periodic density structures areformed around or below 2.5 Rs – the inner edge of the Cor2field of view. Further, we compute the occurrence rate ofperiodic density structures in 10 days of Cor2 images as afunction of location in the solar corona. We find thatperiodic density structures do not occur throughout theentire space-filling volume of the solar wind; rather, thereare particular places where they occur preferentially,suggesting source locations for periodic density structuresin the slow solar wind.Author(s): Nicholeen Viall (NASA Goddard Space Flight Center),Angelos Vourlidas (Naval Research Laboratory)

402.03 – Simulation of S-Web CorridorDynamicsThe higher average charge-state composition and biastowards heavier elements (Zurbuchen et al. 1999) of theslow solar wind suggest that its source is the release ofcoronal plasma from high-temperature, closed-field regions.The S-Web (separatrix web) model for the source of theslow solar wind is based on the conclusion that theapparent multiple coronal holes observed within single-polarity regions are connected by narrow corridors at scalessmaller than the spatial resolution of currentmeasurements. Magnetic field lines from the boundary ofsuch a corridor map to the heliospheric current sheet, whilefield lines from the interior of the corridor map to an arcextending to high latitudes in the heliosphere (Antiochos etal. 2011). In this work, we simulate the dynamics of anS-Web corridor using the Adaptively Refined MHD Solver(ARMS). The objective is to quantify the release of coronalplasma at high heliospheric latitudes and show that thedynamics support the S-Web model as an explanation forthe source of the slow solar wind. We will present resultsfrom our efforts to simulate open-field corridor dynamics,outline plans for further work, and discuss implications forunderstanding the slow solar wind. This work wassupported, in part, by the NASA TR&T and SR&T programs.Author(s): Aleida Young (University of Michigan), Spiro Antiochos(NASA Goddard Space Flight Center), C. DeVore (NASA Goddard SpaceFlight Center), Thomas Zurbuchen (University of Michigan)

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402.04 – MAG4 versus AlternativeTechniques for Forecasting Active-RegionFlare ProductivityMAG4 is a technique of forecasting an active region's rateof production of major flares in the coming few days from afree-magnetic-energy proxy. We present a statisticalmethod of measuring the difference in performancebetween MAG4 and comparable alternative techniques thatforecast an active region’s major-flare productivity fromalternative observed aspects of the active region. Wedemonstrate the method by measuring the difference inperformance between the “Present MAG4” technique andeach of three alternative techniques, called “McIntoshActive-Region Class,” “Total Magnetic Flux,” and “NextMAG4.” We do this by using (1) the MAG4 database ofmagnetograms and major-flare histories of sunspot activeregions, (2) the NOAA table of the major-flare productivityof each of 60 McIntosh active-region classes of sunspotactive regions, and (3) five technique-performance metrics(Heidke Skill Score, True Skill Score, Percent Correct,Probability of Detection, and False Alarm Rate) evaluatedfrom 2000 random two-by-two contingency tables obtainedfrom the databases. We find that (1) Present MAG4 faroutperforms both McIntosh Active-Region Class and TotalMagnetic Flux, (2) Next MAG4 significantly outperformsPresent MAG4, (3) the performance of Next MAG4 isinsensitive to the forward and backward temporal windowsused, in the range of one to a few days, and (4) forecastingfrom the free-energy proxy in combination with either anybroad category of McIntosh active-region classes or anyMount Wilson active-region class gives no significantperformance improvement over forecasting from thefree-energy proxy alone (Present MAG4). Funding for thisresearch came from NASA’s Game Changing DevelopmentProgram, Johnson Space Center’s Space Radiation AnalysisGroup (SRAG), and AFOSR’s Multi-University ResearchInitiative. In particular, funding was facilitated by Dr. DanFry (NASA-JSC) and David Moore (NASA-LaRC).Author(s): David Falconer (NASA/MSFC), Ronald Moore (NASA/MSFC),Abdulnasser Barghouty (NASA's MSFC), Igor Khazanov (UAH)

402.05 – Solar Wind Acceleration: ModelingEffects of Turbulent Heating in Open FluxTubesWe present two self-consistent coronal heating models thatdetermine the properties of the solar wind generated andaccelerated in magnetic field geometries that are open tothe heliosphere. These models require only the radialmagnetic field profile as input. The first code, ZEPHYR(Cranmer et al. 2007) is a 1D MHD code that includes theeffects of turbulent heating created by counter-propagatingAlfven waves rather than relying on empirical heatingfunctions. We present the analysis of a large grid ofmodeled flux tubes (> 400) and the resulting solar windproperties. From the models and results, we recreate theobserved anti-correlation between wind speed at 1 AU andthe so-called expansion factor, a parameterization of themagnetic field profile. We also find that our models followthe same observationally-derived relation betweentemperature at 1 AU and wind speed at 1 AU. We continueour analysis with a newly-developed code written in Pythoncalled TEMPEST (The Efficient Modified-Parker-Equation-Solving Tool) that runs an order of magnitude faster thanZEPHYR due to a set of simplifying relations between theinput magnetic field profile and the temperature and wavereflection coefficient profiles. We present these simplifyingrelations as a useful result in themselves as well as theanti-correlation between wind speed and expansion factoralso found with TEMPEST. Due to the nature of thealgorithm TEMPEST utilizes to find solar wind solutions, wecan effectively separate the two primary ways in whichAlfven waves contribute to solar wind acceleration: 1)heating the surrounding gas through a turbulent cascadeand 2) providing a separate source of wave pressure. Weintend to make TEMPEST easily available to the public andsuggest that TEMPEST can be used as a valuable tool in theforecasting of space weather, either as a stand-alone codeor within an existing modeling framework.Author(s): Lauren Woolsey (Harvard University), Steven Cranmer(Harvard University)

402.06 – A new relaxation technique fordetermining the structure of coronalmagnetic fieldsThe existence of force-free equilibria for arbitrary fieldtopology is a long-standing and unresolved problem (c.f.the 'Parker problem'). We introduce a new numericalmethod for obtaining force-free equilibria. From an initialnon-equilibrium field, an evolution towards a force-free fieldis followed that strictly preserves the magnetic topology(i.e. connectivity and linkage of all magnetic field lines).The method is based on a Lagrangian formulation, andemploys a so-called mimetic method for calculating finitedifferences on the computational mesh. We demonstratethat this provides a significant improvement in theaccuracy of the force-free equilibrium obtained, comparedwith the traditional finite difference approach previouslyemployed. The method is a powerful tool to understand theproperties of coronal loops, which are typically modelled asconsisting of ideal plasma threaded by a force-freemagnetic field. We present some examples of equilibriarepresentative of coronal loops.Author(s): David Pontin (University of Dundee), Simon Candelaresi(University of Dundee), Gunnar Hornig (University of Dundee)

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403 – SPD/LAD Joint Session: Bridging Laboratory and Solar Plasma Studies IMeeting-in-a-Meeting – Staffordshire – 05 Jun 2014 10:00 AM to 11:30 AM

Laboratory astrophysics is the Rosetta Stone that enables astronomers to understand and interpret the cosmos.This joint meeting will focus on the interplay between laboratory astrophysics, plasma physics and solar physics.

Chair(s):Vyacheslav Lukin (Naval Research Laboratory)

403.01 – Role of ambient magnetic field indriving the eruption of an arched laboratorymagnetoplasmaEruptions of arched magnetoplasma structures cover awide spatiotemporal scale on the Sun and drive energeticphenomena such as coronal mass ejections. Due topresence of an electrical-current and associated twist in themagnetic-field, the term “arched magnetic flux rope”(AMFR) is used for these structures. Contemporary modelsof solar eruptions predict that solar AMFRs are confined forrelatively long duration (days to weeks) by ambientmagnetic fields (known as strapping field) before theirsudden eruption. The structure of the ambient-magnetic-field plays an important role in the evolution ofthe confined and erupting solar AMFRs. In a laboratoryplasma experiment, the interaction between an AMFR andits ambient magnetic field has been investigated. The AMFR

(plasma ? ? 10-3, Lundquist number ?102–105, AMFRradius/ion-gyroradius ? 20, B ? 1000 G at footpoints) wasproduced using a LaB6 plasma source in an ambientmagnetoplasma (B ? 0 – 100 G). The ambient magneticfield was oriented normal to the symmetry plane of theAMFR. The experiment runs continuously and generatesreproducible AMFR eruptions with a period of 2 s. Hence,the plasma parameters were recorded with a good

resolution (spatial-resolution/AMFR-length ? 10-2 – 10-3,

temporal-resolution/eruption-time ? 10-3) using computer-controlled movable probes. A fast-CCD camera was utilizedto capture the evolution of the AMFR. The pre-eruptionphase of the AMFR remained quiescent for ? 100 Alfventransit times and the camera images evinced its persistentappearance. In contrast, the post-eruption phase of theAMFR was observed to be associated with significantchanges in its magnetic topology. Our initial results suggestthat linkage of the magnetic-field of the AMFR with theambient magnetoplasma (which is ignored in the models ofsolar eruptions) plays the most important role in theejection of a large flux rope from the leading edge of theAMFR. Implications of these results to actual solar eruptionswill be discussed. References: (1) Tripathi and Gekelman,Phys. Rev. Lett. 105, 075005 (2010) (2) Tripathi andGekelman, Solar Phys. 286, 479 (2013) (Work performed atthe Basic Plasma Science Facility, UCLA and supported byUS DOE and NSF)Author(s): Shreekrishna Tripathi (UCLA), Walter Gekelman (UCLA)

403.02 – Equilibrium features and eruptiveinstabilities in laboratory magnetic fluxrope plasmasOne avenue for connecting laboratory and solar plasmastudies is to carry out laboratory plasma experiments thatserve as a well-diagnosed model for specific solarphenomena. In this paper, we present the latest resultsfrom one such laboratory experiment that is designed toaddress ideal instabilities that drive flux rope eruptions inthe solar corona. The experiment, which utilizes theexisting Magnetic Reconnection Experiment (MRX) atPrinceton Plasma Physics Laboratory, generates a quasi-statically driven line-tied magnetic flux rope in a solar-relevant potential field arcade. The parameters of thepotential field arcade (e.g., its magnitude, orientation, andvertical profile) are systematically scanned in order tostudy their influence on the evolution and possible eruptionof the line-tied flux rope. Each flux rope discharge isdiagnosed using a combination of fast visible light camerasand an in situ 2D magnetic probe array that measures allthree components of the magnetic field over a large cross-section of the plasma. In this paper, we present the firstresults obtained from this new 2D magnetic probe array.With regard to the flux rope equilibrium, non-potentialfeatures such as the formation of a characteristic sigmoidshape and the generation of core toroidal field within theflux rope are studied in detail. With regard to instabilities,the onset and evolution of two key eruptiveinstabilities—the kink and torus instabilities—arequantitatively assessed as a function of the potential fieldarcade parameters and the amount of magnetic energystored in the flux rope. This research is supported by DoEContract Number DE-AC02-09CH11466 and by the NSF/DoECenter for Magnetic Self-Organization (CMSO).Author(s): Clayton Myers (Princeton Plasma Physics Laboratory),Masaaki Yamada (Princeton Plasma Physics Laboratory), Elena Belova(Princeton Plasma Physics Laboratory), Hantao Ji (Princeton Plasma PhysicsLaboratory), Jongsoo Yoo (Princeton Plasma Physics Laboratory), WilliamFox (Princeton Plasma Physics Laboratory)

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403.03 – CME Initiation Driven byVelocity-Shear Kinetic ReconnectionSimulationsIn the standard model for coronal mass ejections (CME)and/or solar flares, the free energy for the event resides inthe strongly sheared magnetic field of a filament channel.The pre-eruption force balance consists of an upward forcedue to the magnetic pressure of the sheared fieldcountered by a downward tension due to overlyingunsheared field. Magnetic reconnection is widely believedto be the mechanism that disrupts this force balance,leading to explosive eruption. For understanding CME/flareinitiation, therefore, it is critical to model the onset ofreconnection that is driven by the build-up of magneticshear. In MHD simulations, the application of amagnetic-field shear is a trivial matter. However, kineticeffects are important in the diffusion region and thus, it isimportant to examine this process with PIC simulations aswell. The implementation of such a driver in PIC methods isnontrivial, however, and indicates the necessity of a truemultiscale model for such processes in the solarenvironment. The field must be sheared self-consistentlyand indirectly to prevent the generation of waves thatdestroy the desired system. In the work presented here, wediscuss methods for applying a velocity shearperpendicular to the plane of reconnection in a system withopen boundary conditions. This material is based uponwork supported by the National Science Foundation underAward No. AGS-1331356.Author(s): Carrie Black (CUA), Spiro Antiochos (NASA/GSFC), JudithKarpen (NASA/GSFC), C. DeVore (NASA/GSFC), Kai Germaschewski (UNH)

403.05 – Spectral Diagnostics of HighResolution Plasmas using AtomDB 3.0AtomDB is a collection of atomic data for modeling X-rayemission from optically thin collisional plasmas. Previousversions of the database have included data required forequilibrium modeling, but have omitted some of the datarequired for modeling inner shell processes which arerelevant to non-equilibrium plasmas. We present the newAtomDB 3.0, which includes significant updates to both theatomic data collection, and the collisional plasma model.We describe the new calculations which have beenpreformed for inner shell ionization and excitation-autoionization, and compare with literature results. As wellas the well known diagnostics of non-equilibrium plasmas,such as the iron K-alpha centroid position, we highlightfeatures in the spectra of ionizing and recombining plasmaswhich will appear in high resolution spectra such as thehigh resolution micro-calorimeter on Astro-H, the Soft X-raySpectrometerAuthor(s): Adam Foster (Harvard Smithsonian, CfA), Randall Smith(Harvard Smithsonian, CfA), Nancy Brickhouse (Harvard Smithsonian, CfA),Li Ji (Purple Mountain Observatory), Hiroya Yamaguchi (NASA GSFC),Timothy Kallman (NASA GSFC), Jörn Wilms (Universität Erlangen-Nürnberg)

403.06 – The Onset of Fast MagneticReconnection in Solar and LaboratoryPlasmasMagnetic reconnection is widely believed to be the physicalprocess underlying explosive activity in both solar andlaboratory plasmas. The question of what determineswhether and when magnetic reconnection will produceexplosive energy release has long been one of the mostimportant problems in all plasma physics. We examine thisproblem using numerical simulations of major solareruptions, coronal mass ejections and eruptive flares.These events are among the most energetic and the bestobserved examples of the onset phenomenon. Ourcalculations show that reconnection in the solar coronainvariably exhibits two distinct phases. First, we observe aninitial slow growth characterized by the appearance of anextended current sheet and magnetic islands, somewhatanalogous to resistive tearing. Eventually, however, thereconnection transitions to an explosive phasecharacterized by well-developed jets and further islandformation. We discuss how these results scale withnumerical refinement level, i.e., effective Lundquistnumber. We conclude that, at least for the case of solarplasmas, fast reconnection onset requires an interactionbetween reconnection and an ideal instability. We discussthe implications of our results for observations of both solarand laboratory plasmas. This work was supported in part bythe NASA TR&T and SR&T Programs.Author(s): Spiro Antiochos (NASA GSFC), C. DeVore (NASA GSFC),Judith Karpen (NASA GSFC), Silvina Guidoni (NASA GSFC)

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404 – Stellar Atmospheres and OutflowsOral Session – St. George AB – 05 Jun 2014 10:00 AM to 11:30 AMChair(s):Derek Buzasi (Florida Gulf Coast University)

404.02 – Radiative 3D Modeling ofConvection of Main-Sequence StarsRecent progress in observational capabilities, andparticularly, the large amount of photometric data fromKepler, require the development of realistic numericalsimulations for data interpretation and validation oftheoretical models. Current state-of-the-art ofcomputational modeling based on first principles makes itpossible to build realistic models of stellar convection zonesand atmospheres, which can take into account chemicalcomposition, effects of radiation, ionization and turbulence.I present large-scale 3D time-dependent radiativehydrodynamics simulations for a series of Kepler-targetstars with masses from 1.01 Ms to 1.52 Ms and effectivetemperature varying from 5780 K to 6982 K, andinvestigate the properties of convection, the surfacestructure and oscillations. For massive A-type stars, thesimulations include the whole outer convection layer andthe overshoot region at the interface with the radiativezone. The simulations reveal that in stars that are moremassive than the Sun, turbulent convection is highlysupersonic and produces multiscale granulation patterns onthe surface. These simulation results also show thatcontrary to current paradigm, turbulent convection plays avery important role in the surface dynamics of A-type stars,and leads to stochastic excitation of acoustic oscillationsobserved by Kepler. I will also discuss the dynamics of theovershooting region and excitation of internal gravitywaves.Author(s): Irina Kitiashvili (NASA Ames Research Center)

404.03 – Temperatures and Radii ofLow-Mass Dwarf Stars Estimated from NearInfrared SpectraWe present estimates of the temperatures and radii of Mdwarfs targeted by the MEarth transiting planet survey. Thefundamental properties of M dwarfs are difficult toconstrain by direct measurement, and we instead useempirical relationships that are based on the strengths ofnear infrared spectral features. We establish ourrelationships for radius and temperature using cool dwarfswith interferometric measurements. Our calibrations usethe equivalent widths of H-band spectral features as tracersof these parameters and have an accuracy of 0.03 solarradii and 60 K for late K to mid M dwarfs. We validate ourmethod by comparing our inferred stellar parameters toabsolute magnitudes, which we calculate using 2MASSmagnitudes and parallaxes from Dittmann et al. (2014). Wealso identify candidate over-luminous objects within oursample, which may be binaries or young stars.Author(s): Elisabeth Newton (Harvard-Smithsonian Center forAstrophysics), David Charbonneau (Harvard-Smithsonian Center forAstrophysics), Jonathan Irwin (Harvard-Smithsonian Center forAstrophysics)

404.04 – A Photometric (griz) MetallicityCalibration for Cool StarsWe present results from a study that uses wide pairs astools for estimating and constraining the metal content ofcool stars from their spectra and broad band colors.Specifically, we will present results that optimize the Mannet al. M dwarf metallicity calibrations (derived using widebinaries) for the optical regime covered by SDSS spectra.We will demonstrate the robustness of the new calibrationsusing a sample of wide, low-mass binaries for which bothcomponents have an SDSS spectrum. Using these newspectroscopic metallicity calibrations, we will presentrelations between the metallicities (from optical spectra)and the Sloan colors derived using more than 20,000 Mdwarfs in the SDSS DR7 spectroscopic catalog. Theserelations have important ramifications for studies ofGalactic chemical evolution, the search for exoplanets andsubdwarfs, and are essential for surveys such asPan-STARRS and LSST, which use griz photometry but haveno spectroscopic component.Author(s): Andrew West (Boston Univ.), James Davenport (Universityof Washington), Saurav Dhital (Embry-Riddle ), Andrew Mann (University ofTexas, Austin), Angela Massey (Boston Univ.)

404.05 – Update on the Stellar SurfaceImaging Project at NPOIWe are working on a project to carry out stellar surfaceimaging at the Navy Precision Optical Interferometer(NPOI). The project is recently funded by the NSF, and willextend the baseline bootstrapping capability of the NPOI to6-station observations in each of the three arms of the NPOIY-configuration array. The project requires thecommissioning of one telescope station beyond what isalready in place or in the process of commissioning, andupgrades to the data acquisition and fringe-trackingsystem. 6-station bootstrapping is not possible with anyother existing interferometer and the number of imageelements is directly related to the length of thebootstrapping chain. Additionally we expect to takeadvantage of wavelength bootstrapping for additionalresolution at short wavelength. Here we will provide anupdate on the project and also discuss some modelingresults showing the kind of imaging resolution that will bepossible and amount of observing time required to producean image.Author(s): Anders Jorgensen (New Mexico Tech), Henrique Schmitt(Naval Research Laboratory), Matthew Landavazo (New Mexico Tech),Brian Sun (New Mexico Tech), David Mozurkewich (Seabrook Engineering),Gerard van Belle (Lowell Observatory), Donald Hutter (Naval ObservatoryFlagstaff Station), J. Armstrong (Naval Research Laboratory), Ellyn Baines(Naval Research Laboratory), James. Clark (Naval Research Laboratory),Kyle Newman (New Mexico Tech), Sergio Restaino (Naval ResearchLaboratory)

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404.06 – Radio Emission from Macroclumpsin Massive Star WindsMassive star winds are understood to be structured.Structures can come in the form of co-rotating interactionregions, which are globally organized flow streams thatthread the winds. Structures can also be stochastic innature, generically referred to as "clumps". The theory forinterpreting the radio emissions from randomly distributedmicroclumps in single star winds is established. Results arepresented here for macroclumping, in which the radiativetransfer is sensitive to the clump geometry. Two cases arecompared: spherical clumps and pancake-like fragments.The geometry of macroclumps can influence the power-lawslope of the long wavelength spectral energy distribution.Author(s): Richard Ignace (East Tennessee State Univ.)

404.07 – TIME-DOMAIN SPECTROSCOPY OFA T TAURI STARHigh resolution optical and near-infrared spectra of TW Hya,the nearest accreting T Tauri star, cover a decade andreveal the substantial changes in accretion and windproperties. Our spectra suggest that the broad near-IR,optical, and far-uv emission lines, centered on the star,originate in a turbulent post-shock region and can undergoscattering by the overlying stellar wind as well asabsorption from infalling material. Stable absorptionfeatures appear in H-alpha, apparently caused by anaccreting column silhouetted in the stellar wind. Thefree-fall velocity of material correlates inversely with thestrength of the post-shock emission, consistent with adipole accretion model. Terminal outflow velocities appearto be directly related to the amount of post-shock emission,giving evidence for an accretion-driven stellar wind.Author(s): Andrea Dupree (Harvard-Smithsonian CfA), NancyBrickhouse (Harvard-Smithsonian CfA), Steven Cranmer (Harvard-Smithsonian CfA), Perry Berlind (Harvard-Smithsonian CfA), Jay Strader(MIchigan State University), Graeme Smith (Lick Observatory)

404.08 – Magnetic Field Structure of theOutflows in NGC1333 IRAS4A ProtostellarCoreWe present the polarization map of CO J = 3-2 line in themolecular outflows launched from NGC1333 IRAS 4Aprotostellar core. The spectral line polarization arises fromthe Goldreich-Kylafis effect, which predicts that thepolarization could be either parallel or perpendicular to themagnetic field direction. To resolve the orientation of COpolarization to magnetic field direction, comparisonsbetween CO polarization and dust polarization are madewith the knowledge that the dust polarization isperpendicular to the magnetic field. We found that withinthe IRAS 4A dusty envelope, the CO J = 3-2 polarizationdirections are mostly perpendicular to the dust polarization,suggesting that the CO polarization is parallel to themagnetic field. The directions of the CO polarization appearto vary smoothly from the dust continuum to thered-shifted lobe of the outflows without any abruptchanges, implying that the CO polarization remains parallelto the magnetic field direction in the outflows. Wespeculate that a helical field may be wrapping around theoutflows, which is consistent with the theoreticalexpectations for outflows associated with a rotating disk.Considering that the CO J = 3-2 polarized emission ismainly contributed from low velocity component of outflowsand the polarization detections distribute around the wall ofoutflows, the magnetic field revealed by CO J = 3-2polarization may be at the wall of outflows and associatedto the interaction between envelope and outflows.Additional observations of line polarization from differentdensity traces are needed to test our proposed scenario.Author(s): Tao-Chung Ching (Harvard-Smithsonian Center forAstrophysics), Shih-Ping Lai (National Tsing Hua University), QizhouZhang (Harvard-Smithsonian Center for Astrophysics)

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405 – Instrumentation, Surveys, and DataOral Session – St. George CD – 05 Jun 2014 10:00 AM to 11:30 AMChair(s):Rosanne Di Stefano (Harvard-Smithsonian CfA)

405.01 – ALTAIR: Precision PhotometricCalibration via Low-Cost Artificial LightSources Above the AtmosphereUnderstanding the properties of dark energy via SNIasurveys (and to a large extent other methods as well)requires unprecedented photometric precision. Laboratoryand solar photometry and radiometry regularly achieveprecisions on the order of parts in ten thousand, butphotometric calibration for non-solar astronomy presentlyremains stuck at the percent or greater level. We presentour project, ALTAIR, sponsored by federal agencies in theU.S. and Canada, to erase this discrepancy, and currentsteps toward achieving laboratory-level photometricprecision for major sky surveys late this decade. Inparticular, we show far- and near-field imaging of theballoon-borne light source we presently launch to altitudesof approximately 20 km, and our initial calibration results(in addition to prior work with a present calibrated source inlow-Earth orbit). Our technique is additionally applicable tomicrowave astronomy. Observation of gravitational wavesin the polarized CMB will similarly require unprecedentedpolarimetric and radiometric precision, and we brieflypresent our plans for a calibrated microwave source abovethe atmosphere as well.Author(s): Justin Albert (Univ. of Victoria), Yorke Brown (DartmouthCollege), Christopher Stubbs (Harvard University), Karun Thanjavur (Univ.of Victoria), Divya Bhatnagar (Univ. of Victoria), J. Paul Kovacs (Univ. ofVictoria), Ryan Thomas (Univ. of Victoria), Claire Cramer (NIST), KeithVanderlinde (University of Toronto), Matt Dobbs (McGill University), ArnoldGaertner (NRC (Institute for National Measurement Standards))

405.02 – A Low Cost and High CapabilityX-ray Grating Spectrometer on the ISSWe present the scientific motivation for a X-ray gratingspectrometer mission to be deployed on the InternationalSpace Station. The primary goals of this mission would beto address the "missing baryon" problem, finally detectingand characterizing the Warm-Hot Intergalactic Medium thatshould exist as filaments threading through intergalacticspace. The mission parameters are similar to those of theIXO X-ray Grating Spectrometer of R=3000 and 1000 sq.cm at 0.5 keV and a bandpass from 0.3-1.0 keV. This wouldalso enable studies of feedback from supermassive blackholes, stellar coronae, and the structure of the interstellarmedium and halo of the Milky Way, amongst other goals.Author(s): Randall Smith (Smithsonian AstrophysicalObservatory), Jay Bookbinder (Smithsonian Astrophysical Observatory),Nancy Brickhouse (Smithsonian Astrophysical Observatory), Adam Foster(Smithsonian Astrophysical Observatory), Robert Petre (NASA's GoddardSpace Flight Center), Andrew Ptak (NASA's Goddard Space Flight Center),Randall McEntaffer (University of Iowa), Mark Bautz (MIT), David Burrows(Pennsylvania State University), Abraham Falcone (Pennsylvania StateUniversity), Joel Bregman (University of Michigan), Jörn Wilms (Friedrich-Alexander Universitaet), Richard Willingale (University of Leicester)

405.03D – An Advanced ScatteredMoonlight ModelIn the current era of precision astronomy, a complete skybackground model is crucial, especially as the telescopesbecome even larger in the next decade. Such a model isneeded for planning observations as well as understandingand correcting the data for the sky background. We havedeveloped a sky model for this purpose, and it is the mostcomplete and universal sky model that we know of to date(Noll et al. 2012). It covers a wide range of wavelengthsfrom 0.3 to 30 microns up to a resolution of 1,000,000 andis instrument independent. Currently it is optimized for thetelescopes at Cerro Paranal and the future site CerroArmazones in Chile. Its original purpose was to improve theESO (European Southern Observatory) ETC (Exposure TimeCalculator) used for predicting exposure times ofobservations with a given signal to noise ratio for a set ofconditions, as part of the Austrian ascension to ESO.Improving the ETC allows for better scheduling andtelescope efficiency, and our new sky model has alreadybeen implemented by ESO. The brightest natural source ofoptical light at night is the Moon, and it is the majorcontributor to the astronomical sky background. We havean improved scattered moonlight model (Jones et al. 2013),where all of the components are computed with physicalprocesses or observational data with less empiricalparametrizations. This model is spectroscopic from 0.3 to2.5 microns and was studied with a FORS1 (Patat et al.2008) and dedicated X-Shooter data set. To our knowledge,this is the first spectroscopic model extending into theinfrared. It includes fully 3-D single and double scatteringcalculations with extrapolations to higher orders (Noll et al.2012), a complex treatment for aerosol scattering (Jones etal. 2013), and a lunar fit based on the ROLO survey (Kieffer& Stone 2005). In addition to its original astronomicalpurpose, since the model is more physical, we can use thescattered moonlight to probe the properties of theatmosphere, such as the distribution of aerosols. Wepresent the current status of the advanced scatteredmoonlight model as well as its performance in the opticaland near-infrared.Author(s): Amy Jones (University of Innsbruck), Stefan Noll(University of Innsbruck), Wolfgang Kausch (University of Innsbruck),Stefan Kimeswenger (University of Innsbruck)

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405.04 – Analysis and Modeling of HSTObservations of the Martian ExosphereWe present an analysis of HST ACS/SBC UV images of theextended hydrogen Lyman alpha emissions from theMartian Exosphere obtained during Oct/Nov 2007 using aradiative transfer code developed by our group. This codecorrects for multiple scattering effects in the atmosphere ofMars. We assume a spherically symmetric atmosphere andhave used the standard Chamberlain approach to modelthe exospheric number density profile. For the lower part ofthe atmosphere, we have used a simplified diffusion modelwith only diffusion of H in carbon di-oxide for constructing anumber density profile of H. By varying the temperature ofthe hydrogen population at the exobase and their numberdensities, we obtain the best fit to the data. We observethat there was a 40% decrease in brightness in the data,which correlates to almost a factor of 10 decrease innumber density in just a span of a month. We also calculatethe escape flux of hydrogen based on the modeled exobasetemperature and number densities, which could then berelated to the amount of water lost from Mars.Author(s): Dolon Bhattacharyya (Boston University), John Clarke(Boston University), Jean-Loup Bertaux (LATMOS), Jean-Yves Chaufray(LATMOS)

405.05 – Analysis of multivariate data:algorithms for physical clustering, withapplication to extended time series data onXRBsWe have explored recent developments in machine learningalgorithms, such as diffusion mapping (Richards et al.2009) which allow us to identify physically similar clustersindependent of prior knowledge. We have successfully usedthis method to separate out different classes of X-raybinaries and of different spectral states within a givensystem. Beyond the immediate astronomical application, astrength of our approach is to offer new and useful insightinto the vast and rapidly growing multi-dimensional datacollections in essentially all fields of investigation, not onlythe astrophysical ones which form our testbed and theimmediate focus of our scientific interest.Author(s): Saeqa Vrtilek (Harvard-Smithsonian, CfA), Bram Boroson(Clayton State University), Joseph Richards (Berkeley)

405.06 – SETI Searches for Radio Transientsfrom Kepler Field Planets and AstropulseCandidatesWe present a search for fast radio transients in targetedobservations of planet candidates in the Kepler Field andcandidate Astropulse sources. Kepler Field observationswere conducted in the band 1.1 and 1.9 GHz using theGreen Bank Telescope in Green Bank, West Virginia and arecentered on 86 stars hosting candidate planets identifiedby the Kepler spacecraft. These stars were chosen based onthe properties of their putative planetary system thought tobe conducive to the development of advanced life,including all systems known (as of May 2011) hosting aKepler Object of Interest (KOI) with a calculated equilibriumtemperature between 230 and 380 K, at least 4 KOIs or aKOI with an inferred radius < 3.0 r_earth and a period > 50d. The Kepler Field is centered at an intermediate galacticlatitude, b = 13.5°, which presents an additionalopportunity to detect signals from the older population ofmillisecond and recycled pulsars located above the galacticplane. The Astropulse radio survey searches for briefwide-band pulses in a 2.5 MHz band centered at 1420 MHzusing commensal data recorded from the Arecibo ALFAreceiver. In early Astropulse analysis, 108 candidatesources were identified that passed a series of testsdesigned to eliminate potential sources of radio frequencyinterference (RFI). We have performed targetedre-observations of these sources at Arecibo over the full(1214–1536 MHz) ALFA band. We have developed asoftware pipeline to locate fast dispersed transients inthese observations, leveraging components of the PRESTOsoftware library. This pipeline consists of finding andremoving RFI, conducting de-dispersion to remove theeffects of dispersion from the interstellar medium (ISM) onthe signal and identifying over- threshold events. We alsoperform de-dispersion at negative dispersion measures,proposed to be a potential technique for intelligentcivilizations to distinguish their emission from naturalsources. We carry out both a periodicity and single-pulsesearch on de-dispersed time series. The outputs from thesesteps are examined to look for both technological andastrophysical sources of impulsive radio emission.Author(s): Abhimat Gautam (University of California, Berkeley),Andrew Siemion (University of California, Berkeley), Eric Korpela(University of California, Berkeley), Jeff Cobb (University of California,Berkeley), Matt Lebofsky (University of California, Berkeley), DanWerthimer (University of California, Berkeley)

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405.07 – The SPT-GMOS SpectroscopicSurvey of Galaxy Clusters Identified By theSouth Pole TelescopeThe SPT-GMOS survey is a large NOAO program that usesthe Gemini Multi-Object Spectrograph (GMOS) on theGemini-South telescope to acquire optical spectroscopy for85 galaxy clusters selected via the Sunyaev-Zel'dovich (SZ)effect from the South Pole Telescope (SPT) microwavebackground survey. The SPT survey is delivering auniformly-selected high-mass cluster sample that isessentially volume-complete beyond z >0.3. The SPT-GMOSfollow-up survey targets a large subset of the full SPTcluster catalog in the redshift range, 0.3 < z < 0.8,providing precision redshifts and velocity dispersionmeasurements for the observed clusters. A primary goal ofthe SPT-SZ galaxy cluster survey is to establishcompetitive, independent constraints on cosmologicalparameters -- including the nature of the dark energy --using measurements of the growth of structure. Achievingthis goal requires a precise understanding of therelationship between the observed SZ signature and theintrinsic cluster mass; uncertainty in this massnormalization is currently the source of the largestsystematic error in SPT's cosmological constraints. TheSPT-GMOS survey contributes to reducing this source ofuncertainty by measuring galaxy cluster masses using thedispersion in the distribution of individual galaxy velocitiesas a probe of the the total matter potential of SPT galaxyclusters. Velocity dispersion measurements from a largecluster sample will average over random projection effects,and will enable the calibration of the SZ-mass scalingrelation, in conjunction with X-ray and lensing data on asmaller sample. The SPT-GMOS survey data also provideslegacy value to the community in the form of a powerfuldataset that can be used to address a wide range ofquestions in galaxy evolution and cluster astrophysics.Author(s): Matthew Bayliss (Harvard-Smithsonian Center forAstrophysics), Christopher Stubbs (Harvard-Smithsonian Center forAstrophysics), Jonathan Ruel (Harvard University)

Contributing teams: South Pole Telescope Collaboration

405.08 – Data Citation in AstronomyMany observatories maintain bibliographies to documenttheir impact and justify their continued funding[1], an effortthat requires humans to discover and curate links betweenthe scientific papers and the data that was used asevidence. The "Best Practices for Creating a TelescopeBibliography", endorsed by IAU C5 WG Libraries,recommends full text searching and human examination ofeach paper.[2] These efforts do not scale well. It is unlikelythat articles published in journals from other discipleswould be found. This is particularly a problem for solarphysics, as solar data has applicability in astrophysics,space weather, and even the earth sciences. As ourscientists are not on the editorial boards of the journalsfrom other disciplines, we can't ensure proper attribution toallow these relationships to be discovered via full textsearching. To better deal with tracking cross-discipline datausage, a number of groups have come up with guidelinesand principles for data citation. In 2012, the NationalAcademy's Board on Research Data and Informationreleased the report "For Attribution-Developing DataAttribution and Citation Practices and Standards" [3] and itwas followed last year by the CODATA-ICSTI report "Out ofCite, Out of Mind".[4] Participants from a number of groupssynthesized a single set of principles for data citation thatcould be endorsed by all groups involved in research.[5]Implementing these principles can help to improve thescientific ecosystem by giving proper attribution to allcontributors to data, improving transparency andreproducability, and making data more easily reusable toboth astronomers and other researchers. We will presentthe Joint Declaration of Data Citation Principles, discuss theimplications of them for astronomical data, and recommendsteps towards implementation. References: [1] Accomazzi,et.al, 2012. http://adsabs.harvard.edu/abs/2012SPIE.8448E..0KA [2] Bishop, Grothkopf &Lagerstrom, 2012. http://iau-commission5.wikispaces.com/file/view/Best+Practices+Final.pdf [3] National ResearchCouncil, 2012. http://www.nap.edu/catalog.php?record_id=13564 [4] CODATA, 2013.http://dx.doi.org/10.2481/dsj.OSOM13-043 [5] FORCE11,2014. http://www.force11.org/datacitationAuthor(s): Joseph Hourcle (Wyle IS)

Contributing teams: Virtual Solar Observatory, FORCE11Data Citation Synthesis Group

406 – Steve Kawaler: The Kepler Mission's "Other" Legacy: The Coming ofAge of Space-based AsteroseismologyPlenary Session – America Ballroom North/Central – 05 Jun 2014 11:40 AM to 12:30 PMChair(s):Paula Szkody (Univ. of Washington)

406.01 – The Kepler Mission's "Other"Legacy: The Coming of Age of Space-basedAsteroseismologyBy awakening us to the amazing abundance of otherplanetary systems, the Kepler mission has been a landmarkin advancing our understanding of the Universe. Thealmost-too-simple basis for these discoveries is accuratephotometry, with high duty cycle, of over 100,000 stars.

Thousands of planetary candidates emerged throughdetection of rare transit events. The data corresponding totransit events, though, is far less than 0.1% of the totalamount of data obtained. The remaining >99.9% of thedata is an exquisite record of the time-domain behavior ofan enormous variety of stars. In this talk I'll discuss theremarkable strides that asteroseismology has been able tomake using the remarkable archive of Kepler photometry.Author(s): Steven Kawaler (Iowa State Univ.)

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407 – Gamma-ray Constraints on the EBL and the IGMF IIMeeting-in-a-Meeting – America Ballroom North/Central – 05 Jun 2014 02:00 PM to 03:30 PM

The light emitted by stars throughout the history of the Universe is encoded in the intensity of the extragalacticbackground light (EBL). Characterization of the EBL and its evolution provides insight into the nature of starformation and galaxy evolution. Direct measurements of the EBL are difficult due to local intense foregroundssuch as the zodiacal light and emission from our own Galaxy. Gamma-ray astronomy provides a valuable indirectprobe of the EBL since high-energy gamma rays may interact with photons of the EBL and generate positron-electron pairs. This introduces an attenuation feature in the spectra of distant gamma-ray sources that can beused to place sensitive constraints on the opacity of the universe to gamma-rays and on the energy density of theEBL. Moreover, the electron-positron pairs can generate an electro-magnetic cascade that reprocessed the initialphoton energy to lower gamma-ray energies producing spectral, spatial and temporal signatures that can be usedto place sensitive constraints on the strength of the intergalactic magnetic field (IGMF). Recent studies usinggamma-ray blazars claimed the detection of EBL-induced absorption signatures consistent with the minimumlevel of EBL intensity expected given the established star formation rate. Thus, there is little room for anadditional, truly diffuse component generated at much higher redshifts. At the same time, other studies based ongamma-ray blazars constrained the strength of the IGMF to be >1e-17 Gauss (depending on the coherent lengthand source activity timescale). Our proposed meeting-in-meeting will focus on up-to-date results and currentlyon-going projects to constrain the strength of the IGMF and further characterize the EBL intensity, its evolution,and its impact on on our understanding of star formation. The first session will cover topics related to the EBL, andits constraints while the second one will deal with the cascade formation, composition and propagation in theintergalactic medium and the derived constraints on the strength of the IGMF.

Chair(s):Luis Reyes (California Polytechnic State Univ. San Luis Obispo)

Organizer(s):Marco Ajello (Berkeley)

407.01 – Must is a Four Letter Word: TheRole of Plasma Instabilities in theIntergalactic Magnetic Field StoryThe detection of inverse Compton halos from cosmologicalTeV sources provide a direct means to constrain theputative intergalactic magnetic field. However, theconverse may not be the case! The fate of the pairsgenerated by TeV gamma rays annihilating on theextragalactic background light is presently unclear, cloudedby the possibility that cosmological scale plasmainstabilities may dominate their energetic evolution. I willbriefly motivate these plasma instabilities theoretically,summarize some empirical evidence that they may beoccurring in practice, and assess their potential impactupon studies of intergalactic magnetic fields.Author(s): Avery Broderick (Perimeter Institute for TheoreticalPhysics)

407.02 – Does the near-infraredextragalactic background light excess comefrom the extragalactic sky?Extragalactic background light (EBL) is one of the mostfundamental observables in the sky. In the optical andinfrared bands, it is widely believed that galaxies explainthe EBL. However, the IRTS and AKARI measurementsreported an excess in the NIR EBL. On the contrary,gamma-ray observations independently confirm that thelevel of EBL is the same as galaxy counts. In this talk, I willreview the current EBL constraints from gamma-rayobservations and discuss their problems. Then, I willintroduce possible explanations for the NIR EBL excess.Author(s): Yoshiyuki Inoue (ISAS/JAXA)

407.03 – Cascaded Gamma Rays as a Probeof Cosmic RaysVery-high-energy (VHE) and ultra-high-energy (UHE)gamma rays from extragalactic sources experienceelectromagnetic cascades during their propagation inintergalactic space. Recent gamma-ray data on TeV blazarsand the diffuse gamma-ray background may have hints ofthe cascade emission, which are especially interesting if itcomes from UHE cosmic rays. I show that cosmic-ray-induced cascades can be discriminated from gamma-ray-induced cascades with detailed gamma-ray spectra. Ialso discuss roles of structured magnetic fields, whichsuppress inverse-Compton pair halos/echoes but lead toguaranteed signals - synchrotron pair halos/echoes.Author(s): Kohta Murase (Institute for Advanced Study)

407.04 – Sensitivity of H.E.S.S. II to Detect aReduced Gamma-ray Opacity Due toPhoton-axion-like Particle OscillationsGamma rays originating from extragalactic sources caninteract with soft energy photons of background radiationfields leading to an attenuation of the primary photon flux.Extensions of the Standard Model of particle physicscommonly predict the existence of light pseudo-scalars.Photons may oscillate into such axion-like particles (ALPs)in ambient magnetic fields. ALPs propagate unimpededover cosmological distances and a conversion back intophotons before reaching Earth can give rise to an increasedgamma-ray flux at high optical depths. The sensitivity todetect this increase with the second phase of the H.E.S.S.Experiment as well as with the future Cherenkov TelescopeArray (CTA) will be presented. For observations compatiblewith the standard predictions for the opacity, limits on thephoton-ALP coupling can be derived.Author(s): Manuel Meyer (OKC / Stockholm University)

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407.05 – Isolating the first populations incosmic infrared background: from Spitzer toEuclidI will review the current measurements of potentialcontribution to the Cosmic Infrared Background (CIB) fromfirst stars and black holes. Intriguing indications of thepossible emissions from these objects have been obtainedover the last several years from CIB fluctuationmeasurements using Spitzer/IRAC deep images. Theuncovered source-subtracted CIB fluctuations substantiallyexceed those from remaining known populations. Thespatial spectrum of these fluctuations is consistent withpopulations clustering according to high-z LCDM model. TheSED of the CIB fluctuations is blue and consistent withemissions produced by hot objects at high z. Cross-correlation analysis with Chandra X-ray data suggests thatthe unresolved CIB and CXB are coherent at a remarkablyhigh level implying fractional abundance of black holes,among the emitters of the CIB, which significantly exceedsthat in known populations. I will also discuss a new CIBproject, LIBRAE (Looking at Infrared Background RadiationAnisotropies with Euclid), planned by NASA and ESA for thefuture Euclid satellite mission. LIBRAE will identify the netemissions from the first stars era, lead to a betterunderstanding of the condition of intergalactic medium atthat epoch, isolate the contributions from the first black

holes and shed light on dust content at those times. Theproject has potentially transformative implications forunderstanding the emergence of the Universe out of the"Dark Ages".Author(s): Alexander Kashlinsky (NASA's GSFC)

407.06 – Secondary Photons and Neutrinosfrom Distant Blazars and the IntergalacticMagnetic FieldsSecondary photons and neutrinos produced in theinteractions of cosmic ray protons and gamma rays emittedby distant Active Galactic Nuclei (AGN) with the photonbackground along the line of sight can reveal a wealth ofnew information about the intergalactic magnetic fields(IGMF), extragalactic background light (EBL), and theacceleration mechanisms of cosmic rays. The secondaryphotons may have already been observed by gamma-raytelescopes. With the inclusion of secondary photons thecurrent upper limits on the extragalactic background lightare significantly weakened and new limits are set for theintergalactic magnetic fields for a wide range of cosmic rayand gamma ray models. Recent results from IceCube mayalso hint at the first observation of secondary neutrinos.Ramifications for the cosmic backgrounds, magnetic fields,and AGN models will be discussed.Author(s): Warren Essey (University of California Los Angeles)

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408 – Corona IIMeeting-in-a-Meeting – America Ballroom South – 05 Jun 2014 02:00 PM to 03:30 PMChair(s):Stephen Bradshaw (Rice University)

408.01 – Observing MHD Waves in the SolarWind Acceleration RegionWe have, for the first time, observed and characterizedcompressive waves propagating both outward and inwardin the outer solar corona above 4 Rs. In addition todetecting the waves, we have used them to measureoutflow in the all-important wind acceleration region.Because the corona is an MHD system, any disturbance inthe corona launches low-frequency waves that propagate atthe familiar MHD speeds and serve to communicate thatdisturbance to other parts of the system. Through carefulfiltration of synoptic STEREO-A/COR-2 data, we have beenable to measure both inbound and outbound waves at alllocations in the solar corona. By measuring in/outasymmetries in the wave characteristics we have been ableto estimate the solar wind acceleration profile. Further, weare able to estimate the location of the Alfvén surface - thehard-to-measure transition between the corona and thesuperalfvénic solar wind, and the boundary at which solarmagnetic field lines transition from "closed" to "open".There is a great deal of work to be done beyond thesepreliminary results, which - it is hoped - open a new avenuefor understanding coronal dynamics and the origin of thesolar wind.Author(s): Craig DeForest (Southwest Research Inst.), DaveMcComas (Southwest Research Institute), Tim Howard (SouthwestResearch Inst.)

408.02 – A Model for the Formation ofFilament Channels on the SunA major unexplained feature of the solar atmosphere is theaccumulation of magnetic shear, in the form of filamentchannels, at photospheric polarity inversion lines (PILs). Inaddition to free energy, this shear also represents magnetichelicity, which is conserved under reconnection.Consequently, the observations raise the question: Why isthe magnetic shear observed to be concentrated alongPILs? Results of 3D MHD simulations using the AdaptivelyRefined MHD Solver (ARMS) are presented that support themagnetic-helicity condensation model of filament-channelformation (Antiochos 2013). In this work, we consider thesupergranular twisting of a quasi-potential flux system thatis bounded by a PIL and contains a coronal hole (CH). Themagnetic helicity injected by the small-scale photosphericmotions is shown to inverse-cascade up to the largestallowable scales that define the closed flux system: the PILand the CH boundary. This process produces field lines thatare both sheared and smooth, and are sheared in oppositesenses at the PIL and the CH, in agreement with Antiochos(2013). The accumulated helicity and shear flux are shownto be in excellent quantitative agreement with the helicity-condensation model. We present a detailed analysis of thesimulation, including comparisons of our analytical andnumerical results, and discuss their implications forobservations. This work was supported, in part, by theNASA TR&T and SR&T programs.Author(s): Kalman Knizhnik (NASA Goddard Space Flight Center),Spiro Antiochos (NASA Goddard Space Flight Center), C. DeVore (NASAGoddard Space Flight Center)

408.03 – Magnetic Untwisting in Jets thatGo into the Outer Solar Corona in PolarCoronal HolesWe present results from a study of 14 jets that wereobserved in SDO/AIA EUV movies to erupt in the Sun’s polarcoronal holes. These jets were similar to the many otherjets that erupt in coronal holes, but reached higher than thevast majority, high enough to be observed in the outercorona beyond 2 solar radii from Sun center by theSOHO/LASCO/C2 coronagraph. We illustrate thecharacteristic structure and motion of these high-reachingjets by showing observations of two representative jets. Wefind that (1) the speed of the jet front from the base of thecorona out to 2-3 solar radii is typically several times thesound speed in jets in coronal holes, (2) each high-reachingjet displays unusually large rotation about its axis (spin) asit erupts, and (3) in the outer corona, many jets displaylateral swaying and bending of the jet axis with anamplitude of a few degrees and a period of order 1 hour.From these observations we infer that these jets aremagnetically driven, propose that the driver is a magnetic-untwisting wave that is basically a large-amplitude(non-linear) torsional Alfven wave that is put into the openmagnetic field in the jet by interchange reconnection as thejet erupts, and estimate that the magnetic-untwisting waveloses most of its energy before reaching the outer corona.These observations of high-reaching coronal jets suggestthat the torsional magnetic waves observed in Type-IIspicules can similarly dissipate in the corona and therebypower much of the coronal heating in coronal holes andquiet regions. This work is funded by the NASA/SMDHeliophysics Division’s Living With a Star Targeted Research& Technology Program.Author(s): Ronald Moore (NASA's MSFC), Alphonse Sterling (NASA'sMSFC), David Falconer (NASA's MSFC)

408.04 – Mass Flows in a Prominence Spineas Observed in EUVWe analyze a quiescent prominence observed by the SolarDynamics Observatory's Atmospheric Imaging Assemblywith a focus on mass and energy flows in the spinemeasured using Lyman continuum absorption. This is thefirst time this sort of analysis has been applied with anemphasis on individual features and flows in a quiescentprominence. The prominence, observed on 2010 Sept. 28,is detectable in most AIA wavebands in absorption and/oremission. Flows along the spine exhibit horizontal bands5-10 arcsec wide and kinetic energy fluxes consistent withquiet sun coronal heating estimates. For a discrete movingfeature we estimate a mass of a few times 10^11 g. Wediscuss the implications of our derived properties formodels of prominence dynamics, in particular the thermalnon-equilibrium model. This project was supported byNASA's LWS TR&T program.Author(s): Therese Kucera (NASA's GSFC), Holly Gilbert (NASA'sGSFC), Judith Karpen (NASA's GSFC)

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408.05 – Modeling the multi-ion structure ofthe solar coronaThe solar corona is typically observed in EUV by SDO/AIAand other instruments using the heavy ion emission linessuch as Fe IX, Fe XII, and other ion emission lines. However,the relative (to protons) abundance of the emitting ions isvery low and the collisional coupling between the Fe ionsand electrons decreases rapidly with height in the lowcorona, while gravitational settling may become significantin quiescent long-lived magnetic structures, such asstreamers. Thus, the structure of the weakly collisionalsolar corona imaged in Fe IX (and other heavy ions) maydiffer significantly from the structure of the main electron-proton constituents of the corona. The electron structure isobserved by white light coronagraphs, and during solareclipses in the low corona. I present the results ofmulti-fluid modeling of coronal streamers and othermagnetic structures that demonstrate the effects of weakcoupling between the heavy ions and the coronal electron-proton components, and show that the multi-ion coronalstructure must be taken into account in interpretation ofEUV observations.Author(s): Leon Ofman (Catholic University and NASA's GSFC),

Elena Provornikova (Catholic University and NASA's GSFC), Tongjiang Wang(Catholic University and NASA's GSFC)

408.06 – Observations of Alfvèn WaveDamping in the Quiet CoronaWe present a measurement of line widths in quiet Sunregions of the corona. The non-thermal line width isproportional to the amplitude of Alfvèn waves. Using aPotential Field Source Surface (PFSS) magnetic field modelto identify magnetic field lines, we trace the evolution ofline widths along the inferred field lines. In order to mitigateline of sight effects, we select regions that are isothermaland where the field lines remain oriented close toperpendicular to the line of sight. Our results indicate thatthe waves are damped starting at a height that is positivelycorrelated with the overall length of the loop. That is, forlonger loops, the damping occurs starting at a largerheight. This suggests that heating of quiet Sun loops occursover a region centered on the loop top and extends over alarge fraction of the loop. We estimate that there is enoughenergy flux in waves injected at the base of quiet Sunregions to account for coronal heating in such structures.Author(s): Michael Hahn (Columbia University), Daniel Savin(Columbia University)

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409 – SPD/LAD Joint Session: Bridging Laboratory and Solar Plasma Studies IIMeeting-in-a-Meeting – Staffordshire – 05 Jun 2014 02:00 PM to 03:30 PM

Laboratory astrophysics is the Rosetta Stone that enables astronomers to understand and interpret the cosmos.This joint meeting will focus on the interplay between laboratory astrophysics, plasma physics and solar physics.

Chair(s):Daniel Savin (Columbia Astrophysics Lab.)

409.01 – On Cosmic Ray PropagationCosmic ray propagation is diffusive because of pitch anglescattering by waves. We demonstrate that if thehigh-amplitude magnetic turbulence with (delta B)/B ~ 1 ispresent on top of the mean field gradient, the diffusionbecomes asymmetric. As an example, we solve thisdiffusion problem in one dimension analytically with aMarkov chain analysis. The cosmic ray density markedlydiffers from the standard diffusion prediction. The equationfor the continuous limit is also derived, which showslimitations of the convection-diffusion equation. There is aninteresting connection of this problem to laboratoryexperimental studies of particle transport in multi-mirrormachines. The implications of the results are discussed.Supported by grant DOE grant DE-FG02-07ER54940 andNSF grant AST-1209665.Author(s): Mikhail Medvedev (University of Kansas)

409.02 – Role of Z-pinches in magneticreconnection in space plasmasA generally accepted scenario of magnetic reconnection inspace plasmas is the breakage of magnetic field lines inX-points. In laboratory, reconnection is widely studied inpinches, current channels embedded into twisted magneticfields. No model of magnetic reconnection in space plasmasconsiders both null-points and pinches as peers. We haveperformed a particle-in-cell simulation of magneticreconnection in a three-dimensional configuration wherenull-points are present initially, and Z-pinches are formedduring the simulation. The X-points are relatively stable,and no substantial energy dissipation is associated withthem. On the contrary, turbulent magnetic reconnectiondriven by kinking of the pinches causes the magneticenergy to decay at a rate of 1.5% per ion gyro period.Current channels and twisted magnetic fields areubiquitous in turbulent space plasmas, so pinches can beresponsible for the observed high magnetic reconnectionrates.Author(s): Vyacheslav Olshevsky (KU Leuven), Giovanni Lapenta (KULeuven), Stefano Markidis (KTH Royal Institute of Technology), AndreyDivin (Swedish Institute of Space Physics)

409.03 – Two LANL laboratory astrophysicsexperimentsTwo laboratory experiments are described that have beenbuilt at Los Alamos (LANL) to gain access to a wide range offundamental plasma physics issues germane to astro,space, and fusion plasmas. The over arching theme ismagnetized plasma dynamics which includes significantcurrents, MHD forces and instabilities, magnetic fieldcreation and annihilation, sheared flows and shocks. TheRelaxation Scaling Experiment (RSX) creates current sheetsand flux ropes that exhibit fully 3D dynamics, and can kink,bounce, merge and reconnect, shred, and reform incomplicated ways. Recent movies from a large data setdescribe the 3D magnetic structure of a driven anddissipative single flux rope that spontaneously selfsaturates a kink instability. Examples of a coherent shearflow dynamo driven by colliding flux ropes will also beshown. The Magnetized Shock Experiment (MSX) uses Fieldreversed configuration (FRC) experimental hardware thatforms and ejects FRCs at 150km/sec. This is sufficient todrive a collision less magnetized shock when stagnated intoa mirror stopping field region with Alfven Mach numberMA=3 so that super critical shocks can be studied. We arebuilding a plasmoid accelerator to drive Mach numbers MA>> 3 to access solar wind and more exotic astrophysicalregimes. Unique features of this experiment include accessto parallel, oblique and perpendicular shocks, shock regionmuch larger than ion gyro radii and ion inertial length, roomfor turbulence, and large magnetic and fluid Reynoldsnumbers. *DOE Office of Fusion Energy Sciences underLANS contract DE-AC52-06NA25396, NASA GeospaceNNHIOA044I, Basic, Center for Magnetic Self OrganizationAuthor(s): Thomas Intrator (Los Alamos Natl Lab), Thomas Weber(Los Alamos Natl Lab), Yan Feng (Los Alamos Natl Lab), Trevor Hutchinson(Los Alamos Natl Lab), John Dunn (Los Alamos Natl Lab), Cihan Akcay (LosAlamos Natl Lab)

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409.04 – Magnetic structure of sites ofbraiding in Hi-C active regionHigh-resolution Coronal Imager (Hi-C) observations of anactive region (AR) corona, at a spatial resolution of 0.2arcsec, have offered the first direct evidence of field linesbraiding, which could deliver sufficient energy to heat theAR corona by current dissipation via magneticreconnection, a proposal given by Parker three decadesago. The energy required to heat the corona must betransported from the photosphere along the field lines. Themechanism that drives the energy transport to the coronais not yet fully understood. To investigate simultaneousmagnetic and intensity structure in and around the AR indetail, we use SDO/HMI+AIA data of + / - 2 hours aroundthe 5 minute Hi-C flight. In the case of the QS, work doneby convection/granulation on the inter-granular feet of thecoronal field lines probably translates into the heatobserved in the corona. In the case of the AR, as here,there could be flux emergence, cancellation/submergence,or shear flows generating large stress and tension incoronal field loops which is released as heat in the corona.However, to the best of our knowledge, there is noobservational evidence available to these processes. Weinvestigate the changes taking place in the photosphericfeet of the magnetic field involved with brightenings in theHi-C AR corona. Using HMI 45s magnetograms of four hourswe find that, out of the two Hi-C sub-regions where thebraiding of field lines were recently detected, fluxemergence takes place in one region and flux cancellationin the other. The field in these sub-regions are highlysheared and have apparent high speed plasma flows attheir feet. Therefore, shearing flows plausibly power muchof the coronal and transition region heating in these areasof the AR. In addition, the presence of large fluxemergence/cancellation strongly suggests that the workdone by these processes on the pre-existing field alsodrives much of the observed heating. For this work, SKTand CEA were supported by an appointment to the NASAPostdoctoral Program at the NASA Marshall Space FlightCenter, administered by Oak Ridge Associated Universitiesthrough a contract with NASA, and AW and RLM weresupported by funding from the Living With a Star TargetedResearch and Technology Program of the HeliophysicsDivision of NASA's Science Mission Directorate.Author(s): Sanjiv Tiwari (NASA's MSFC), Caroline Alexander (NASA'sMSFC), Amy Winebarger (NASA's MSFC), Ronald Moore (NASA's MSFC)

409.05 – Alfven Wave Collisions, theFundamental Building Block of PlasmaTurbulence: Theoretical, Numerical, AndExperimental VerificationTurbulence plays a key role in the evolution of space andastrophysical plasmas, mediating the transfer of energyfrom large-scale turbulent motions to small scales wherethe turbulent energy is ultimately converted to plasmaheat. In the solar corona, turbulence is believed to play akey, yet incompletely understood, role in the heating of theplasma to temperatures nearly three orders of magnitudehotter than the photosphere. The cascade of energy fromlarge to small scales is mediated by the nonlinearinteraction between counterpropagating Alfven waves, orAlfven wave "collisions," the fundamental building block ofastrophysical plasma turbulence. First, I present ananalytical solution for the nonlinear evolution of Alfvenwave collisions that elucidates the physical mechanism bywhich energy is transferred from large to small scales.Next, I show that the analytical solution is validated usingnonlinear gyrokinetic simulations of weakly collisionalplasma turbulence. Finally, I present the experimentalverification of the physics of Alfven wave collisions in thelaboratory using the Large Plasma Device (LAPD) at UCLA.Author(s): Gregory Howes (University of Iowa), Kevin Nielson(University of Iowa), Dereth Drake (Valdosta State University ), JamesSchroeder (University of Iowa), Frederick Skiff (University of Iowa), CraigKletzing (University of Iowa), Troy Carter (University of California)

409.06 – Hybrid Kinetic and RadiativeHydrodynamic Simulations of Solar Flaresand Comparison With MultiwavelengthObservationsWe present a unified simulation which combines twophysical processes: how the particles are accelerated andthe energy is transported along a coronal loop, and how theatmosphere responds. The “flare” code from StanfordUniversity (Petrosian et al, 2001) models the stochasticacceleration and transport of particles and radiation ofsolar flares. It includes pitch angle diffusion and energyloss, and computes collisional heating to the backgroundplasma and bremsstrahlung emission along the loop. Theradiative hydrodynamic RADYN Code (Carlsson et al, 1992,1996; Allred et al, 2005) computes the energy transport bythe injected non-thermal electrons at the top of a 1Dcoronal loop. Recently, we have combined the two codes byupdating the non-thermal heating in the RADYN code fromthe "flare" code, allowing us to develop a self-consistentsimulation. In addition, we can now model more realisticallythe multi-wavelength emission of solar flares and compareit with observations, e.g., at optical wavelengths from IBISat the Dunn Solar Telescope and in X-rays from RHESSI. Thehigh resolution UV observations from the recently launchedIRIS imaging spectrograph will be particularly useful in thisregard. These will allow us to compare numerically modeledand observed emissions of solar flares in several lines usingmore robust simulations than possible before.Author(s): Fatima Rubio Da Costa (Stanford University), VahePetrosian (Stanford University), Wei Liu (Stanford University), MatsCarlsson (University of Oslo), Lucia Kleint (University of Applied SciencesNorth Western Switzerland )

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410 – AGN, QSO, BlazarsOral Session – St. George AB – 05 Jun 2014 02:00 PM to 03:30 PMChair(s):Laura Brenneman (Harvard-Smithsonian Center for Astrophysics)

410.01 – Searching for Obscured Quasarswith WISE and the Southern African LargeTelescopeWe present the results of an optical spectroscopic survey ofa sample of 43 obscured quasars identified on the basis oftheir mid-infrared emission detected by the Wide-FieldInfrared Survey Explorer (WISE). Optical spectra for thissurvey were obtained using the Robert Stobie Spectrograph(RSS) on the Southern African Large Telescope (SALT). Ourtarget objects are selected to have red WISE colorscharacteristic of AGN, as well as red optical to mid-IR colorsindicating that the optical/UV AGN continuum is obscuredby dust. We obtain secure redshifts for the majority of theobjects that comprise our sample (37/43), and find thatsources that are bright in the WISE 22?m band are typicallyat moderate redshift (0.2-0.5) while 22?m fainter sourcesare at higher redshifts. The majority of the sources havenarrow emission lines, with optical colors and emission lineratios of our WISE-selected sources that are consistent withthe locus of AGN on the color-excitation diagram betweenrest-frame g - z color and [NeIII]?3869 / [OII]??3726+3729line ratio. These results verify the efficiency of WISE colorcriteria in selecting luminous obscured AGN.Author(s): Kevin Hainline (Dartmouth College), Ryan Hickox(Dartmouth College), Christopher Carroll (Dartmouth College), Adam Myers(University of Wyoming), Laura Trouille (Northwestern University), MichaelDiPompeo (University of Wyoming)

410.02 – Through the Ring of Fire: A Studyof the Origin of Orphan Gamma-ray Flaresin BlazarsBlazars exhibit flares across the electromagnetic spectrum.Many gamma-ray flares are highly correlated with flaresdetected at optical wavelengths; however, a small subsetappear to occur in isolation, with no counterpart in theother wave bands. These "orphan" gamma-ray flareschallenge current models of blazar variability, most ofwhich are unable to reproduce this type of behavior. Wepresent numerical calculations of the time variableemission of a blazar based on a proposal by Marscher et al.(2010) to explain such events. In this model, a plasmoid("blob") consisting of a power-law distribution of electronspropagates relativistically along the spine of a blazar jetand passes through a synchrotron emitting ring of electronsrepresenting a shocked portion of the jet sheath. This ringsupplies a source of seed photons that are inverse-Compton scattered by the electrons in the moving blob. Asthe blob approaches the ring, the photon density in theco-moving frame of the plasma increases, resulting in anorphan gamma-ray flare that then dissipates as the blobpasses through and then moves away from the ring. Themodel includes the effects of radiative cooling and aspatially varying magnetic field. Support for the plausibilityof this model is provided by observations by Marscher etal.(2010) of an isolated gamma-ray flare that wascorrelated with the passage of a superluminal knot throughthe inner jet of quasar PKS 1510-089. Synthetic light-curvesproduced by this new model are compared to the observedlight-curves from this event. In addition, we presentpolarimetric observations that point to the existence of ajet sheath in the quasar 3C 273. A rough estimate of thebolometric luminosity of the sheath results in a value of~10^45 erg s^-1 (~ 10% of the jet luminosity). Thisinferred sheath luminosity indicates that the jet sheath in3C 273 can provide a significant source of seed photonsthat need to be taken into account when modeling thenon-thermal emission due to inverse-Compton scatteringprocesses. Funding for this research was provided by anNSERC PGS D2 Doctoral Fellowship and NASA under FermiGuest Investigator grants NNX12AO79G and NNX12AO59G.Author(s): Nicholas MacDonald (Boston Univ.), Alan Marscher (BostonUniv.), Svetlana Jorstad (St. Petersburg University), Manasvita Joshi(Boston Univ.)

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410.03 – Using Long-term Optical-InfraredColor Variability to Probe the Disk-JetConnection in BlazarsWe undertook a 5 year, multiwavelength program toobserve a sample of blazars in various Fermi $\gamma$-raystates, using the Small and Medium Aperture ResearchTelescope System (SMARTS) 1.3 m + ANDICAM instrumentin Cerro Tololo, Chile. We present near daily, optical-infrared(OIR) color variability to constrain competing emission inthe OIR wavebands, presumably from the accretion diskand highly variable jet. The main results of previousshort-term color variability studies are reproduced in mostcases, namely that BL Lacs are bluer when brighter andFSRQs are redder when brighter. However, we extend thisinterpretation by providing a self-consistent way to explainblazars that did not behave as predicted by the existingdichotomy in blazar color variability. We show that overlong timescales, patterns emerge in the OIR color variabilitythat are not seen on shorter timescales due to the selectioneffects introduced by only observing blazars in$\gamma$-ray flaring states. By observing a large sampleof blazars on up to 5 year timescales, we show that theseshort-term color variability 'snapshots' can be incorporatedinto a more comprehensive understanding of blazar OIRcolor variability, and by extension the contribution ofnon-thermal jet flux in the OIR regime. Finally, we addresshow long-term OIR color variability can constrain thedisk-jet interaction in blazars.Author(s): Jedidah Isler (Syracuse University), Charles Bailyn (YaleUniversity), Paolo Coppi (Yale University), Imran Hasan (Yale University),Emily MacPherson (Yale University), Michelle Buxton (Yale University), C.Urry (Yale University)

Contributing teams: Yale-SMARTS

410.04 – Jet Feedback on the InterstellarMedium of the Radio Galaxy 3C 293We present a 70 ks Chandra observation of the radio galaxy3C 293. This galaxy belongs to the class of molecularhydrogen emission galaxies (MOHEGs) that have veryluminous emission from warm molecular hydrogen. In thecase of radio galaxies, the molecular gas appears to beheated by jet-driven ISM turbulence. 3C 293 contains 3.7 x10^9 solar masses of shock-heated, 100 K molecularhydrogen in an extended 10 kpc scale region. WithChandra, we observe emission from the jets both within thehost galaxy and outside of the galaxy, along the 100 kpcradio jets. Some of the soft X-rays are coincident with theradio hotspots, but one X-ray emitting feature isanti-coincident with the radio emission. We model the X-rayspectra of the nucleus, the inner jets, and the X-rayfeatures along the extended radio jets. Both the nucleusand the inner jets show evidence of 10^7 K shock-heatedgas. The kinetic power of the jets is more than sufficient toheat the X-ray emitting gas, which serves as a reservoir ofthermal and turbulent energy to maintain the molecularhydrogen emission over a time scale of 10^7 years.Author(s): Lauranne Lanz (California Institute of Technology),Patrick Ogle (California Institute of Technology), Philip Appleton (CaliforniaInstitute of Technology), Bjorn Emonts (Australia Telescope NationalFacility), Daniel Evans (National Science Foundation)

410.05 – DASCH detection of a ~17y QPO inthe 100y light curve of 3C273The Digital Access to a Sky Century @ Harvard (DASCH)project is digitizing the ~500,000 plates in the Harvardplate collection which are (primarily) direct images rangingfrom 4 x 5deg through 30 x 40deg and covering full skyfrom 1885 - 1992 (see dasch.rc.fas.harvard.edu). Thisresults in ~1000 - 3000 images of any object. Astrometricpositions for each resolved object are measured on eachplate to 0.3 -3arcsec (depending on plate scale) and B bandphotometry is derived to +/-0.1mag using the APASSsurvey for spatially dependent photometric calibration andcolor corrections. Limiting magnitudes are typically B = 13 -17. We report the 100y lightcurve (~1100 points) of thebright quasar 3C273 and the analysis of its ~1magvariability on timescales ranging from days to decades. Wehave used generalized Lomb-Scargle techniques, whichhandle the inherently unevenly spaced data sampling andseasonal gaps, to investigate the preferred variabilitytimescales and possible quasi-periodic oscillations (QPOs)present in this unique dataset. An advantage of the DASCHdata and processing is the ready availability of a largecomparison sample of nearby non-variable objects(foreground stars) of comparable magnitude which thendirectly measure the noise due to both photometric errorsand (particularly) the uneven sampling. The generalized L-Speriodogram shows significant excess (vs. field stars)power on several well defined timescales, the mostprominent being at ~17.2y. The full power spectrum isderived using the CARMA model fitting technique describedby Kelly et al, arXiv:1402.5978 and will be compared with avariety of models for the origin of the ~17y QPO as well asthe significance of the several shorter timescale features.Models for the physical origin of the QPO features arediscussed, including optical emission from precession of thejet in 3C273. Prospects for detection of similar longtermvariability in other bright AGN with DASCH, when the fullproduction scanning is available (only 12% of the plates arenow scanned), are also discussed. DASCH gratefullyacknowledges support from NSF grants AST-0407380,AST-0909073, and AST-1313370.Author(s): Jonathan Grindlay (Harvard-Smithsonian, CfA), GeorgeMiller (Harvard-Smithsonian, CfA), Aneta Siemiginowska (Harvard-Smithsonian, CfA), Edward Los (Harvard-Smithsonian, CfA), Brandon Kelly(UCSB), Sumin Tang (UCSB)

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410.06 – Mid-Infrared Selected Quasars I:Virial Black Hole Mass and Eddington RatiosWe provide a catalog of 391 mid-infrared-selected (MIR,24?m) broad-emission-line (BEL, type 1) quasars in the 20square deg SWIRE Lockman Hole field. This quasar sampleis selected in the MIR from Spitzer MIPS with S24 > 0.4mJy,and jointly with an optical magnitude limit of r (AB)= 22.5.The catalog is based on MMT spectroscopy to select BELquasars, and extends the SDSS coverage to faintermagnitudes and a more complete quasar population. TheMIR-selected quasar sample peaks at z ?1.4, and shows asignificant and constant (20%) fraction of objects withextended SDSS photometry, previously missed by the SDSSoptical point source dominant color selection. This samplealso recovers a significant population of z < 3 quasars at i> 19.1, previously dropped by SDSS for efficiencyconsideration. We also investigate the continuumluminosity and line profile of these MIR quasars, estimatetheir virial black hole masses, and provide the Eddingtonratios. The SMBH mass shows evidence of downsizing,though the Eddington ratios remain constant at 1 < z < 4.Compared to point sources in the same redshift range,extended sources at z < 1 show systematically lowerEddington ratios. The catalog and spectra will be publiclyavailable online.Author(s): Yu Dai (Harvard-Smithsonian Center for Astrophysics),Martin Elvis (Harvard-Smithsonian Center for Astrophysics), JacquelineBergeron (Institut d?Astrophysique de Paris), Giovanni Fazio (Harvard-Smithsonian Center for Astrophysics), Jiasheng Huang (Harvard-Smithsonian Center for Astrophysics), Belinda Wilkes (Harvard-Smithsonian Center for Astrophysics), Christopher Willmar (University ofArizona)

410.07 – Using Quasars fromSDSS-III/SEQUELS to CharacterizeSDSS-IV/eBOSS selectionAs part of the fourth incarnation of the Sloan Digital SkySurvey (SDSS-IV) the extended Baryon OscillationSpectroscopic Survey (eBOSS) will compile opticalspectroscopy of by far the largest sample of quasars todate. A homogeneous sample selection that takesadvantage of SDSS ugriz imaging coupled with informationfrom the WISE 3.4 micron and 4.6 micron bands will targetabout three-quarters of a million total quasars over an areaof 7500 square degrees across the North and SouthGalactic caps. Some eBOSS quasars will have existingspectroscopy from earlier versions of the SDSS, butspectroscopy of over half-a-million new quasars will beobtained over a wide range of redshifts (mostly z > 0.9)close to the faint limits of the SDSS imaging (r < 22). Aprecursor survey to eBOSS, the Sloan Extended QUasar,ELG and LRG Survey (SEQUELS) has already beenconducted over ~500 square degrees near the NorthGalactic Cap. I will discuss target selection for eBOSS, andthe results of applying this target selection as part ofSEQUELS. ADM was partially supported through NSF Grant1211112 and NASA ADAP award NNX12AE38GAuthor(s): Adam Myers (University of Wyoming), Eric Armengaud(CEA-Saclay), Jo Bovy (Institute for Advanced Study), W. Brandt (ThePennsylvania State University), Etienne Burtin (CEA-Saclay), JohanComparat (LAM/CNRS), Kyle Dawson (University of Utah), TimotheeDelubac (EPFL/Observatoire de Sauverny), Shirley Ho (Carnegie MellonUniversity), Jean-Paul Kneib (EPFL/Observatoire de Sauverny), Dustin Lang(Carnegie Mellon University), Cameron McBride (CfA/Harvard), Ian McGreer(University of Arizona), Jeffrey Newman (University of Pittsburgh), NathaliePalanque-Delabrouille (CEA-Saclay), Isabelle Paris (Universidad de Chile),William Percival (University of Portsmouth), Patrick Petitjean (Institutd?Astrophysique de Paris), Ashley Ross (University of Portsmouth), DavidSchlegel (Lawrence Berkeley National Laboratory), Yue Shen (CarnegieObservatories), Christophe Yeche (CEA-Saclay)

Contributing teams: The SDSS-III Collaboration, TheSDSS-IV Collaboration

410.08 – Unveiling Obscured AGN with X-raySpectral AnalysisWith the recent advent of physically motivated,self-consistent X-ray models, the circumnuclear mediumenshrouding AGN can now be investigated inunprecedented detail. We applied these models to 19 SDSS[OIII] 5007 Angstrom selected Type 2 AGN, where 9 arelocal Seyfert 2 galaxies and 10 are more luminous anddistant Type 2 quasars. For the first time in a sample ofAGN, we constrained both the line-of-sight and globalcolumn densities, finding that over half (11/19) are heavilyobscured or Compton-thick (NH > 10^23 cm^-2). Fourobjects have different global from line-of-sight columndensities. When correcting the observed X-ray luminositiesfor obscuration, the L_x/L_[OIII] ratio for these Type 2 AGNis essentially identical to the Seyfert 1 (i.e., unabsorbedAGN) value, which is consistent with both parameterscleanly probing AGN emission.Author(s): Stephanie LaMassa (Yale University), Tahir Yaqoob (NASA-GSFC), Andrew Ptak (NASA-GSFC), Jianjun Jia (The Johns HopkinsUniversity), Timothy Heckman (The Johns Hopkins University), PoshakGandhi (Durham University), C. Urry (Yale University)

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410.09 – The Cosmic Evolution of Fermi BLLacertae ObjectsIt has been notoriously difficult in the past to measure thecosmological evolution of BL Lacs because of thechallenges related to measure their redshift. Extensiveoptical follow-up observations of a sample of ~200 Fermi-detected BL Lac objects have provided much-neededredshift information for many of them. This stands as thelargest and most complete sample of BL Lacs available inthe literature and was used to determine the cosmological

properties of this elusive source class. This talk will reviewthe cosmic evolution of BL Lacs and discuss the link to theirsiblings flat-spectrum radio quasars (FSRQs). Evidencesuggests that BL Lacs of the high-synchrotron peaked classmight be an accretion-starved end-state of an earliermerger-driven gas-rich phase.Author(s): Marco Ajello (Clemson), Dario Gasparrini (ASI Space DataCenter), Roger Romani (Stanford University), Michael Shaw (StanfordUniversity)

Contributing teams: Fermi-LAT team

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411 – Relativistic Astrophysics, Gravitational Lenses & WavesOral Session – St. George CD – 05 Jun 2014 02:00 PM to 03:30 PMChair(s):James Aguirre (University of Pennsylvania)

411.01 – Microlensing with HubbleMicrolensing can be used to study dark matter, galacticstructure, and to search for extra-solar planets. However, asignificant problem with microlensing is the massdetermination of the lens. Typically, microlensing eventsprovides only a single measured quantity that depends onthe lens mass, the Einstein angle crossing time, ?, whichalso depends on the distances to the lens and source aswell as the relative transverse velocity. Thus, it is difficult toderive unique mass estimates for the lens. Non-degeneratesolutions are possible, as was shown by Alcock et al. forMACHO LMC-5, when the source and lens can be resolved.It may be possible to distinguish between the lens andsource by re-observing a microlensing candidate years afterthe first observation. As it turns out, a substantial numberof fields containing microlensing events have beenobserved by the Hubble Space Telescope (HST). Wecurrently have identified over 180 possible matches tolensing events. In many of these cases, there was a timedifference of years between the HST observation (orobservations) and the ground-based detection. We presentinitial results from our archival program and discuss theimplications for future studies.Author(s): Idan Ginsburg (Center for Astrophysics), Rosanne DiStefano (Center for Astrophysics), Sebastien Lepine (Georgia StateUniversity), Francis Primini (Center for Astrophysics), Antonia Oprescu(Center for Astrophysics), Ben Tunbridge (Center for Astrophysics)

411.02 – An overview of LIGO and Virgo --status and plansInterferometric gravitational-wave detectors, the mostsensitive position meters ever operated, aim to detect themotion of massive bodies throughout the universe bypushing precision measurement to the standard quantumlimit and beyond. A global network of these detectors iscurrently under construction, promising unprecedentedsensitivity and the ability to determine the sky position ofany detected signals. I will describe the current status andexpected performance of this network with a focus onlimiting noise sources and the techniques currently beingdeveloped to combat them.Author(s): John Miller (MIT)

Contributing teams: LIGO-Virgo Collaboration

411.03 – Sky localization of gravitationalwave sources in the early years ofAdvanced LIGO and VirgoAdvanced LIGO and Virgo, the ground-based km-scale laserinterferometers for gravitational wave detection, will startcollecting data in 2015-2016. Many of the most promisingsources of gravitational waves, such as compact binarycoalescences, are also expected to emit in theelectromagnetic spectrum. The detection of theelectromagnetic counterpart to a gravitational-wave sourceshould help answering open questions, e.g. if compactbinary systems are the progenitors of short gamma raybursts. In this talk I will report on sky localizationcapabilities for signals emitted by binary neutron stars,focusing on the first two years of activity of Advanced LIGOand Virgo.Author(s): Salvatore Vitale (MIT), Leo Singer (Caltech), Larry Price(Caltech), Benjamin Farr (Northwester University ), Alex Urban (Universityof Wisconsin-Milwaukee), Chris Pankow (University of Wisconsin-Milwaukee), John Veitch (University of Birmingham), Will Farr (University ofBirmingham), Chad Hanna (Pennsylvania State University ), Kipp Cannon(Canadian Institute for Theoretical Astrophysics), Tom Downes (Universityof Wisconsin-Milwaukee), Philip Graff (NASA Goddard Space Flight Center),Carl-Johan Haster (University of Birmingham), Ilya Mandel (University ofBirmingham), Trevor Sidery (University of Birmingham), Alberto Vecchio(University of Birmingham)

411.04 – Expected sky localizationcapabilities for un-modeledgravitaitonal-wave transients in 2015 and2016The LIGOs and Virgo, advanced ground-basedGravitational-wave detectors, are expected to begincollecting science data in the next few years. With firstdetections expected to follow, it is important to quantifyhow well gravitational-wave transients can be localized onthe sky. This is crucial for correctly identifyingelectromagnetic counterparts as well as understandinggravitational-wave physics and source populations. Wepresent a study of sky localization capabilities for severalsearches for un-modeled gravitational-wave signals. Wefocus on Coherent WaveBurst, a maximum likelihoodalgorithm used by gravitational-wave observatories, andLALInferenceBurst, a Monte Carlo Markov Chain parameterestimation algorithm developed to recover transientsignals. Because these searches are sensitive tounexpected sources of radiation, it is vital to correctlylocalize them on the sky to facilitate electromagnetic followup. Furthermore, we focus on the first few years of theadvanced detector era, when we expect to only have twooperational detectors (2015) and when we expect to havethree operational detectors (2016). These detectorconfigurations can produce significantly different skylocalizations, which we quantify in detail.Author(s): Reed Essick (MIT), Salvatore Vitale (MIT), ErotokritosKatsavounidis (MIT), Sergey Klimenko (University of Florida), GabrieleVedovato (University of Trento)

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411.05 – Measuring the spin of black holesin binary systems using gravitational wavesCompact binary coalescences are promising sources ofgravitational waves for ground based detectors. Binarysystems containing one or two spinning black holes areparticularly interesting due to spin-orbit (and eventualspin-spin) interactions, and these systems present anopportunity to measure spins directly through gravitationalwave observations. In this talk we analyze simulatedsignals emitted by spinning binaries with several values ofmasses, spins, orientation, and signal-to-noise ratio. Wefind estimates for the measurement accuracy of the spinmagnitudes and spin angles and analyze how thesemeasurement capabilities vary with the binaries'orientations.Author(s): Ryan Lynch (MIT)

411.06 – Multi-messenger Observations ofGravitational-Wave Sources in theAdvanced Detectors EraIn the near future the advanced ground-basedgravitational-wave detectors will open a new direction inobservational astronomy. Detection of gravitational waveswill allow us to perform the first unambiguous observationsof coalescence of compact binaries consisting of neutronstars and stellar-mass black holes. The multi-messengerand multi-wavelength observations of such transientgravitational-wave events with other instruments will helpus to identify their location, understand their environmentand examine their hypothesized connection with the shortgamma-ray bursts. They will also provide a wealth ofcomplementary data from which we can infer newinformation about compact objects and various physicalprocesses taking place during or after the coalescence. Inaddition to coalescing binaries, we should also be preparedto discover completely new classes of gravitational-wavetransients, for which verification and understanding themulti-messenger observations at other wavelengths wouldbe equally important. In this talk I will give an overview ofthe observing plans for the advanced detectors in thesecond half of this decade, and their projected capabilitiesin discovering and localizing the transientgravitational-wave sources. I will describe the mainchallenges in performing the multi-messenger observationsof such sources and what we do to overcome them inpreparation for future observational campaigns. I willconclude by presenting the initiative led by the LIGO andVirgo collaborations to involve a wider astronomicalcommunity in the follow-up multi-messenger observationsstarting with the very first advanced detectors science runin 2015.Author(s): Ruslan Vaulin (MIT)

Contributing teams: The LIGO Scientific Collaboration,The Virgo Collaboration

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412 – Supernovae and White DwarfsOral Session – Gloucester, 2nd Floor – 05 Jun 2014 02:00 PM to 03:30 PMChair(s):Lynn Matthews (MIT Haystack Observatory)

412.01 – Measuring the Spin Rate Change ofV455 AndV455 And (HS2331+3905) is an unusual cataclysmicvariable that displays both an orbital (81 min) and a spin(67s) period, thus classifying it as an Intermediate Polar.The magnetic field of this interacting white dwarf channelsthe accretion stream from the secondary towards the whitedwarf poles, which become heated, resulting in the visibilityof both the spin period and its harmonic in the lightcurvesof V455 And. Our group has been observing this objectsince its discovery. In 2007, V455 And underwent a largeamplitude dwarf nova outburst. This provided an uniqueopportunity to gauge the overall angular momentum gaindue to its long-term accretion as well as its 2007 outburst.Using these data that span the timebase of a decade from2003 to 2013, we constrain the rate of change of its spinperiod with time to be dP/dt = (-6.8 +/- 4.8) 10^{-15} s/sfor the spin period of 67.61970396 +/- 0.00000024s. Wewere able to fit the pre- and post-outburst data togetherbecause we did not find any evidence for a significantdiscontinuity in the O-C diagram due to the 2007 outburst.This implies that the magnetic field couples the angularmomentum gain to the white dwarf interior. Our next goalis to constrain the angular momentum evolution of anon-magnetic accreting white dwarf to probe how the gainin angular momentum due to accretion is transferred to theenvelope and core of the white dwarf.Author(s): Paula Szkody (Univ. of Washington), Anjum Mukadam(Univ. of Washington), Boris Gaensicke (University of Warwick), JJ Hermes(McDonald Observatory)

412.02 – Testing the Hibernation Model forCataclysmic Variable Evolution withVery-Long Very-Well-Sampled Light Curvesof Old NovaeThe Hibernation Model for the evolution of cataclysmicvariables predicts that old novae should be fading at a rateof order one-magnitude-per-century or so, with nomechanism for the accretion rate to significantly increase.This old prediction has been basically impossible to testdue to the absence of very long term light curves where allthe magnitudes have been placed onto a single consistentphotometric system. However, in the past year, I havecreated very-long and very-well sampled light curves forold novae with the magnitudes fully corrected into theJohnson B & V system. I have these long light curves for QCyg (Nova Cyg 1876), V603 Aql (Nova Aql 1918), GK Per(Nova Per 1901), BT Mon (Nova Mon 1939), and QZ Aur(Nova Aur 1964) plus its orbital period change across its1964 eruption. The comparison with the Hibernationprediction is mixed.Author(s): Bradley Schaefer (Louisiana State Univ.)

412.03 – The Post-merger MagnetizedEvolution of White Dwarf Binaries: TheDouble-degenerate Channel ofSub-Chandrasekhar Type Ia Supernovae andthe Formation of Magnetized White DwarfsType Ia supernovae (SNe Ia) play a crucial role asstandardizable cosmological candles, though the nature oftheir progenitors is a subject of active investigation. Recentobservational and theoretical work has pointed to mergingwhite dwarf binaries, referred to as the double-degeneratechannel, as the possible progenitor systems for some SNeIa. Additionally, recent theoretical work suggests thatmergers which fail to detonate may produce magnetized,rapidly rotating white dwarfs. In this presentation, I willpresent the first multidimensional simulations of thepost-merger evolution of white dwarf binaries to include theeffect of the magnetic field. In these systems, the two whitedwarfs complete a final merger on a dynamical timescale,and are tidally disrupted, producing a rapidly rotating whitedwarf merger surrounded by a hot corona and a thick,differentially rotating disk. The disk is strongly susceptibleto the magnetorotational instability (MRI), and I willdemonstrate that this leads to the rapid growth of aninitially dynamically weak magnetic field in the disk, thespin-down of the white dwarf merger, and to thesubsequent central ignition of the white dwarf merger.Additionally, these magnetized models exhibit new featuresnot present in prior hydrodynamic studies of white dwarfmergers, including the development of MRI turbulence inthe hot disk, magnetized outflows carrying a significantfraction of the disk mass, and the magnetization of thewhite dwarf merger to field strengths ~2 × 10^8 G. Idiscuss the impact of these findings on the origins,circumstellar media, and observed properties of SNe Ia andmagnetized white dwarfs.Author(s): Robert Fisher (University of Massachusetts Dartmouth),Enríque Garcia-Berro (Universitat Politècnica de Catalunya), Suoqing Ji(University of Massachusetts Dartmouth), Rahul Kashyap (University ofMassachusetts Dartmouth), Gabriela Aznar-Siguán (Universitat Politècnicade Catalunya), Petros Tzeferacos (University of Chicago), Dongwook Lee(University of Chicago), Pablo Lorén-Aguilar (University of Exeter)

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412.04 – N103B: A Type Ia Supernova withCircumstellar Interaction and Kepler's OlderCousin?A small but growing subclass of Type Ia supernovae showssigns of interaction with material in a circumstellar medium(CSM). Among Type Ia supernova remnants (SNRs), only theremnant of Kepler's supernova has been shown to beinteracting with a dense CSM, likely the result of significantpre-supernova mass loss from the progenitor system. Wereport here on Spitzer infrared observations of N103B, aType Ia remnant in the Large Magellanic Cloudapproximately 1,000 years old, that also shows signs of adense CSM. Spectroscopy of the remnant shows acontinuum from warm dust heated in the post-shockenvironment. Model fits to the data give a post-shock gasdensity of 45 cm$^{-3}$, virtually identical to what is seenin Kepler. The dust spectrum is dominated by silicategrains, implying an oxygen-rich environment in the stellaratmosphere of at least one star in the progenitor system. Inlight of the densities we derive from IR fits, we examineX-ray spectra and find that while a significant amount ofoxygen is present, the oxygen is consistent with an origin inthe CSM, not the ejecta. Detailed morphologicalcomparisons with X-ray images show a connection betweendust emission and oxygen-rich material, while opticalcomparisons clearly show that dust originates in the fast,non-radiative, Balmer-dominated shocks, and not theslower, radiative shocks. We see no obvious evidence forfreshly formed ejecta dust. Again, N103B shares all of thesecharacteristics with Kepler. We conclude that N103B is anolder analog of Kepler, and thus only the second knownmember of the subclass of Type Ia SNRs interacting withdense CSM material long after their explosion.Author(s): Brian Williams (NASA Goddard), Kazimierz Borkowski(North Carolina State University), Stephen Reynolds (North Carolina StateUniversity), Parviz Ghavamian (Towson University), Knox Long (SpaceTelescope Science Institute), P. Winkler (Middlebury College), JohnRaymond (Harvard CfA), Ravi Sankrit (SOFIA/USRA), Sean Hendrick(Millersville University), William Blair (Johns Hopkins University)

412.05 – Multi-wavelength analysis ofsupernova remnant MSH11-61ADue to its centrally bright X-ray morphology and limbbrightened radio profile, supernova remnant (SNR)MSH11-61A (G290.1-0.8) is classified as mixed morphology.The evolutionary sequence which leads to this centrallybright X-ray morphology is not well understood andcurrently different models can only explain some of thefeatures seen in individual cases. In this analysis wepresent a study of MSH11-61A using archival Suzaku data.Our preliminary results indicate enhanced abundances, aspreviously suggested by ASCA observations and we derivethe associated age, energy and ambient density of theremnant using models that we constructed in an attempt toreproduce the observed X-ray properties. Additionally,MSH11-61A is thought to be interacting with a molecularcloud towards the west/south west of the remnant. Asobservations of thermal and non-thermal emission of SNRshave provided increasing support in favour of cosmic raysbeing accelerated at the shock front of the remnant, SNRsknown to be interacting with molecular clouds provide aneffective target for detecting and studying gamma-rays.Using 64 months of Fermi-LAT gamma-ray data, we performa spatial and spectral analysis of the gamma-ray emissionin the region of this remnant, allowing us to constrain theorigin of the detected emission.Author(s): Katie Auchettl (Monash University), Patrick Slane (HarvardSmithsonian Center for Astrophysics), Daniel Castro (Kavli Institute forAstrophysics & Space Research)

412.06 – Non Parametric Determination ofAcceleration Characteristics in SupernovaShocks Based on Spectra of Cosmic Raysand Remnant RadiationWe have developed an inversion method for determinationof the characteristics of the acceleration mechanismdirectly and non-parametrically from observations, incontrast to the usual forward fitting of parametric modelvariables to observations. This is done in the frame work ofthe so-called leaky box model of acceleration, valid forisotropic momentum distribution and for volume integratedcharacteristics in a finite acceleration site. We considerboth acceleration by shocks and stochastic accelerationwhere turbulence plays the primary role to determine theacceleration, scattering and escape rates. Assuming aknowledge of the background plasma the model hasessentially two unknown parameters, namely themomentum and pitch angle scattering diffusioncoefficients, which can be evaluated given two independentspectral observations. These coefficients are obtaineddirectly from the spectrum of radiation from the supernovaremnants (SNRs), which gives the spectrum of acceleratedparticles, and the observed spectrum of cosmic rays (CRs),which are related to the spectrum of particles escaping theSNRs. The results obtained from application of this methodwill be presented.Author(s): Vahe Petrosian (Stanford Univ.), Qingrong Chen (StanfordUniv.)

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412.07 – Constraints on the dimensionlessage of the Universe from Pan-STARRSsupernovaeWe present the constraints on the dimensionless age of theuniverse H_o t_o determined from the latest compilation ofType Ia Supernovae (SN Ia) of the Pan-STARRS1 MediumDeep Survey, combined with low-z supernovae from theCfA, Carnegie, and other sources. The cosmological fit to

these SN Ia, assuming a spatially flat universe as suggested

by Planck, yields a value of H_o t_o = 1.039 +0.04-0.05. In

this talk we briefly discuss the procedure and implicationsof this result.Author(s): Arturo Avelino (Harvard-Smithsonian Center forAstrophysics), Robert Kirshner (Harvard-Smithsonian Center forAstrophysics), Daniel Scolnic (Department of Physics and Astronomy, JohnsHopkins University)

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Authors IndexAbbett, William P. 123.47Abel, Nicholas 419.01Abramenko, Valentyna 323.01Adams, Elizabeth A. 222.01Adams, Fred C. 108.01Adams, Joseph D. 223.01Adams, Joseph D 213.02DAdelman, Saul J. 322.16Agudo, Ivan 221.19Aguirre, James E. 318.02Ahn, Kwangsu 123.53, 323.08Ahrendts, Gary 321.04Ajello, Marco 401.04, 410.09Ajoku, Chukwuemeka 119.03Akcay, Cihan 409.03Akeson, Rachel L. 120.10Akiyama, Sachiko 303.06Alaoui, Meriem 123.33Albert, Justin 405.01Alexander, Caroline 312.06Alexander, Caroline 323.20, 409.04Alexander, Kate Denham 121.17Ali, Babar 220.12Allen, Branden 122.16, 321.11Allen, Lori 121.15, 215.03, 220.12Aller, Hugh D. 221.09Aller, Margo F. 221.09Allers, Katelyn N. 322.13Allred, Joel C. 313.05Allured, Ryan 418.02Almeyda, Triana 221.17Almgren, Ann 121.01Altrock, Richard C. 323.32Amouzou, Ernest C. 218.29Andersen, Jan Marie 322.11Anderson, Craig 417.03Anderson, Jay 122.04, 122.05Anderson, Mark 123.57Anderson-Huang, Lawrence 420.07Andrade-Santos, Felipe 206.03Andrews, Sean M. 322.01, 322.21,322.22Aniol, Peter 323.57Anthony, Francys 322.08Antiochos, Spiro K. 121.10, 121.11,218.16, 218.37, 323.51, 402.03,403.03, 403.06, 408.02Antolin, Patrick 313.03Antoniou, Vallia 319.05Antunes, Alexander 107.01Anupama, G. C 122.18Apai, Daniel 120.14Appleton, Philip N. 410.04Araya, Claudia 223.03Arcand, Kimberly K. 316.04Archibald, Anne 121.12Archontis, Vasilis 312.02Arge, Charles 323.23, 323.36Arimoto, Nobuo 223.13Armengaud, Eric 410.07Armstrong, J. T. 404.05Arshakian, Tigran 221.15Arulanantham, Nicole 223.04

Asa'd, Randa 314.01Aschwanden, Markus J. 123.06,123.37Asfaw, Tilaye Tadesse 323.26Asgari-Targhi, Mahboubeh 323.25Ashby, Matthew 206.05, 213.03,215.07, 319.07Atek, Hakim 417.06Atwood, Jenny 122.18Atwood, Shane 123.55Auchettl, Katie 412.05Aufdenberg, Jason P. 322.19Aulanier, Guillaume 312.02Avelino, Arturo 412.07Avrett, Eugene H. 422.02Axelrod, Tim S. 319.04Aya, Higuchi 223.02Ayres, Thomas R. 323.12Aznar-Siguán, Gabriela 412.03Babyak, Zachary 421.05Baggett, Sylvia M. 122.03, 122.04Bailey, Jim 305.02Bailyn, Charles D. 122.20, 410.03Bain, Hazel 123.11, 323.67, 323.68,323.69Baines, Ellyn K. 404.05Baker, Robert 122.16Bala, Vishal 221.08Balasubramaniam, K. S. 123.05Baldner, Charles 202.05, 218.19Baldwin, Austin 219.18Bale, Stuart D 323.67Balick, Bruce 121.07, 121.08, 121.09,121.14Ballard, Sarah 314.05Baragiola, Raul , 119.12Barclay, Thomas 113.06, 301.07Bardelli, Sandro 417.08Barghouty, Abdulnasser F 402.04Barker, Timothy 321.04Barnes, Arnold 122.11Barnes, Graham 112.03, 218.15Barrett, Douglas 421.06Barron-Santella, Angelica 320.07Barry, D. J 223.11Barthelmy, Scott Douglas 122.16,421.04Bastien, Fabienne A. 102.03Basu, Sarbani 218.19Batalha, Natalie M. 113.04Batalha, Natalie M 120.06Baudin, Frédéric 218.17Bauer, Franz E. 121.18Bauer, Wendy Hagen 322.20Baumgartner, Wayne H. 421.04Bautista, Manuel 106.04, 119.03,221.18Bautz, Mark W. 122.13, 122.14,321.11, 405.02Bayliss, Matthew 405.07Beauchamp, Jack L 214.04Beck, Christian 112.02Becker, A. 119.07

Becker, Samantha Lauren 320.07Becklin, Eric E. 213.02D, 213.03Beckmann, Simon 418.03Beeson, Charlie 321.10Beichman, Charles A. 311.05Belanger, Zachary 319.01, 319.02Belikov, Ruslan 311.07Bell, John 121.01Bellinger, Earl 219.07Belova, Elena V 403.02Beltz-Mohrmann, Gillian 219.05Bender, Ralf 213.06Benedict, G. Fritz 420.06Benkendorf, Barry 219.11Benner, Aaron 421.05Bennett, Philip D. 322.20Bercik, David J 123.47Berendsen, Marni 316.02Berger, Edo 121.13, 421.08Berger, Thomas 212.01, 313.03Bergeron, Jacqueline 410.06Bergonio, Justin 214.03Berlicki, Arek 123.39Berlind, Perry L. 404.07Berta-Thompson, Zachory K. 120.15Bertaux, Jean-Loup 321.06, 405.04Bertello, Luca 218.31Bertin, Mathieu 205.04Betzler, Alberto 421.06Bhatnagar, Divya 405.01Bhattacharjee, Amitava 305.03Bhattacharyya, Dolon 405.04Bian, Nicolas 123.22Bianchi, Luciana 306.01Bieryla, Allyson 121.17, 320.05Biller, Beth 301.01Binzel, Richard P. 321.08, 321.09,321.11Birch, Aaron 202.01, 202.06, 218.07Biretta, John A. 122.04Birnstiel, Tilman 322.22, 322.23Bischoff, Addi 119.06Biteau, Jonathan 401.03Bizzarro, Martin 102.05Black, Carrie 121.10, 121.11, 403.03Blacketer, Melissa 219.03Blair, William P. 306.01, 412.04Blakeslee, John 322.02Blancard, C. 305.02Blanchard, Peter 121.17Blanton, Elizabeth L. 206.05, 222.02,222.05Bloomfield, D. Shaun 123.16Blum, Lauren 107.02Blumenthal, Kelly 318.12Bobra, Monica 123.52Bochanski, John J. 322.15Boerner, Paul 323.22Bogart, Richard S. 202.05, 218.05,218.19, 218.23Bogdan, Akos 222.03Bohlin, Ralph 319.04Bolatto, Alberto D. 215.04, 220.03

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Bonafede, Annalisa 206.04Bond, Nicholas A. 417.06Bondarenko, Anton 305.01Boogert, Adwin 418.04Bookbinder, Jay A. 122.14, 405.02Bord, Donald J. 219.02Borkowski, Kazimierz J. 412.04Bormanis, Mikus 107.01Borncamp, David 122.02Boroson, Bram S. 405.05Bostroem, K. Azalee 122.07, 122.08Boswell, Josiah S 119.03Bourque, Matthew 122.04Bouvier, Jerome 223.03Bovy, Jo 221.01, 410.07Bowens-Rubin, Rachel 415.02Bower, Geoffrey C. 204.07Bowers, Ariel 122.03Bradley, Richard F. 318.06Bradshaw, Stephen 302.06Brainerd, Tereasa G. 318.12Brandt, W. Niel 410.07Brannon, Sean 111.02Braun, Douglas 202.01, 202.06,218.07, 218.15Bregman, Joel N. 122.14, 405.02Breitfellner, Michel 119.06Brenneman, Laura 221.12, 221.13Brenneman, Laura 221.12, 221.13Brenner, Michael P 311.07Brickhouse, Nancy S. 122.14, 403.05,404.07, 405.02Briggs, John W. 421.02Brighenti, Fabrizio 417.08Brinchmann, Jarle 222.01Britt, Chris 219.18Broderick, Avery 407.01Broderick, Jess 204.05Brodie, Jean P. 222.08Brodwin, Mark 206.05Brosius, Jeffrey W. 312.04, 323.39Brotherton, Michael S. 221.04Brown, Benjamin 211.04Brown, Gregory V. 106.02Brown, Thomas M. 417.06Brown, Yorke 405.01Browning, Benjamin 318.10Brugarolas, Paul 311.07Brunner, Robert J. 423.03Bryans, Paul 422.03Bryant, Aaron 418.03Bryden, Geoffrey 301.04, 311.07Bryk, William 120.21Bryson, Kathryn 119.06Bryson, Steve 120.06, 120.08Buchhave, Lars A 102.03Buchhave, Lars A. 102.05, 120.19Bucik, Radoslav 123.18Buell, James F. 121.06Buhr, H. 119.07Buitrago-Casas, Juan Camilo 123.38Bulbul, Esra 222.02Bulbul, G. Esra 206.04Burdette, Daniel P 423.02Burgasser, Adam J. 322.13Burke, Christopher J. 113.04, 120.01,

120.03, 120.06Burke, Douglas J. 417.03Burke-Spolaor, Sarah 204.07Burnham, Jill 122.16Burrows, Adam Seth 201.03Burrows, David N. 122.14, 405.02Burt, Brian J. 321.08, 321.09Burtin, Etienne 410.07Burtseva, Olga 123.28Bush, Rock 218.25, 218.33Buson, Sara 401.04Butler, Bryan J. 204.07Buxton, Michelle 122.20, 410.03Buzasi, Derek L. 322.06Byrne, Jason 323.57Cadmus, Robert R. 219.04Cady, Eric 311.06Cahoy, Kerri Lynn 102.02, 122.09,311.07Caldwell, Douglas A. 120.06, 120.07Caldwell, Martin 123.57Caldwell, Nelson 223.13Cally, Paul S 112.04Cameron, Chris 219.06Campbell, Amy M 221.11Candelaresi, Simon 402.06Canfield, Richard C. 123.49Canizares, Claude R 421.01Cannon, Kipp 411.03Cao, Wenda 123.04, 123.09, 123.53,323.08Caplan, Ron 323.36Capozzi, Diego 206.08Carey, Sean J. 213.03, 220.09Cargile, Phillip 121.05Carlson, Mackenzie 219.13Carlsson, Mats 123.39, 313.02, 313.05,313.06, 409.06Carpenter, John M. 322.22Carroll, Carla 221.07Carroll, Christopher M 410.01Carry, Benoit 321.09Carson, Joseph 113.08Carter, Troy A 409.05Carveth, Carol 321.06Case, Michael 418.04Casey, Caitlin 206.07Cash, Webster C. 311.06Cashman, Lauren 220.06, 220.07Casini, Roberto 323.24Cason, Andy 421.06Caspi, Amir 123.02, 123.07, 123.13,123.64Castro, Daniel 412.05Castro, Victor H 320.06Catanzarite, Joseph 120.05, 120.09Catanzarite, Joseph 120.04Cauzzi, Gianna 123.39, 302.01,323.04Chaboyer, Brian C. 420.05, 420.06Chae, Jongchul 323.08Chakrabarti, Sukanya 417.02Chakrabarti, Supriya 113.09, 120.13,122.09Chakrabarti, Supriya 122.10, 220.01,311.07

Chamberlin, Phillip C. 123.15Champagne, Arthur E. 315.01Chandler, Claire J. 322.22Chang, Philip 417.02Chang, William 123.57Chang, Yih C 114.03Change, Po-Yu 305.03Chaplin, William J 102.03Charbonneau, David 113.01, 113.03,120.15, 120.20, 404.03Charlton, Jane C. 215.08Chatterjee, Piyali 212.03Chatterjee, Suchetana 221.05Chaufray, Jean-Yves 321.06, 405.04Chavushyan, Vahram 221.15Cheimets, Peter 123.56Chen, Qingrong 104.02, 412.06,414.04Chen, Ruizhu 202.03Chen, Xi 120.10Chen, Yao 123.40, 218.02, 303.03Cheng, Jianxia 218.32Chengalur, Jayaram N. 222.01Cheung, Mark 323.22Cheung, Teddy 221.10Chiang, Eugene 419.08Ching, Tao-Chung 404.08Chintzoglou, Georgios 323.28Cho, Kyung-Suk 323.08Chodas, Mark 321.11Chornock, Ryan 121.13, 421.08Chou, Amy 123.36Christe, Steven 123.61, 123.62,123.64, 218.39Christiansen, Jessie 113.04, 113.05,120.10Chun, Mark Richard 318.10Chun, Sang-Hyun 223.08Chung, Chul 223.13Churazov, Eugene 222.03Ciardi, David R. 120.10, 322.07Ciccozzi, Katelyn 219.14Cirtain, Jonathan W. 323.11, 323.20Civano, Francesca M. 221.02, 222.12Clark, E. 305.01Clark, James. H 404.05Clarke, Bruce 120.06, 120.07Clarke, John T. 321.05, 321.06, 405.04Clarke, Melanie 418.04Clarke, Tracy E. 222.05Clarkson, William I. 219.02, 219.19,319.01, 319.02Clarkson, William I. 219.02, 219.19,319.01, 319.02Claver, Chuck F. 122.17Clayton, Geoffrey C. 110.05, 219.12,322.17Clemens, Dan P. 220.06, 220.07,220.08, 222.04, 223.11Clyne, Elisabeth 219.02Clyne, Elizabeth 319.01Cobb, Jeff 405.06Cody, Ann Marie 223.04Coe, Dan A. 417.06Cohen, Daniel Parke 123.51Cohen, Seth A. 206.02

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Colbert, James W. 417.06Colditz, Sebastian 418.03Colegrove, Owen 218.09Colgan, J. 305.02Collins, Karen A 219.08Combes, Francoise 417.08Cominsky, Lynn R. 122.23Comparat, Johan 410.07Connors, Jake 415.02Conroy, Charlie 222.08Constantin, Carmen 305.01Contreras, Cesar 114.04Cook, Timothy 113.09, 120.13,122.09, 122.10, 220.01Cook, William 122.16Coppi, Bruno 403.04Coppi, Paolo S. 410.03Cordero, Maria Jose 223.03Coriat, Mickaël 204.05Corradi, Romano 121.07, 121.08,121.09, 121.14Cortes, Paulo 223.02Cosse, Ph 305.02Cotera, Angela 223.05Cotton, William D. 213.01Coughlin, Jeffrey 113.04Coughlin, Michael 122.17Coulter, Roy 112.01Courrier, Hans 218.49, 414.06Couvidat, Sebastien 123.11, 123.31,218.25, 422.07Cox, Colin 122.02Cramer, Alexander 123.61Cramer, Claire 405.01Cranmer, Steven R. 211.06, 323.56,402.01, 402.05, 404.07Crepp, Justin R. 210.03Criscuoli, Serena 123.51, 323.61Crone-Odekon, Mary 222.10Crouch, Ashley D. 202.06, 218.07Cudworth, Kyle M. 223.09Culver, Roger B. 219.01Curtis, Jason L. 223.10, 322.03Czekala, Ian 322.01D'Abrusco, Raffaele 223.12D'Angelo, Gennaro 120.18D'Cruz, Noella L. 320.10Dage, Kristen 219.02, 219.19Dahlen, Tomas 122.03Dai, Yu Sophia 410.06, 417.06Dai, Yu 111.03Daigneau, Peter 122.14Dalba, Paul A. 122.12Dalmasse, Kevin 312.02Dame, Thomas M. 415.01, 415.02Danowski, Meredith E. 220.01Davenport, James R. A. 404.04Davey, Alisdair R. 218.18, 218.46David, Laurence P 222.03David, Laurence P. 417.08Davila, Joseph M. 123.57, 123.59,323.30, 323.54Davis, Allen B. 323.16Daw, Adrian N. 312.04, 313.05,323.06, 323.39Dawson, Kyle S. 410.07

De Mello, Duilia F. 417.06de Mooij, Ernst 416.03de Oliveira, Nelson 119.04De Pontieu, Bart 313.01, 313.02,313.04, 313.05, 313.06, 323.05,323.70De Pree, Christopher G. 223.06de Propris, Roberto 319.01De Ruette, Nathalie 119.05, 119.11de Val-Borro, Miguel 219.15Deady, Michelle 420.07Deb, Sukanta 219.07Debes, John H. 122.07, 122.08DeBoer, David 318.01DeForest, Craig 218.26, 323.63,408.01DeGrave, Kyle 218.03Dekens, Frank 311.07Delubac, Timothee 410.07DeLuca, Ed 313.06, 323.20DeLuca, Edward E. 123.56, 211.03,218.20, 218.22, 218.29, 303.01,303.02, 323.25DeMeo, Francesca E. 321.08, 321.09Demianski, Marek 323.16Deng, Na 123.04Dennis, Brian R. 111.01, 123.23,323.49DePalma, David 421.01Derekas, Aliz 219.06DeRosa, Marc L. 123.19, 323.19Desjardins, Tyler D. 314.02Dessart, Luc 121.16Deustua, Susana E. 122.03, 319.04Devlin, Thomas 123.57DeVore, C. Richard 104.05, 121.10,121.11, 218.16, 218.37, 323.51,402.03, 403.03, 403.06, 408.02DeWitt, Curtis N. 418.04Dhital, Saurav 102.09, 219.16, 404.04Di Stefano, Carlos 413.01Di Stefano, Rosanne 120.21, 300.01,319.03, 411.01Diaz, Ernesto 418.05Dillon, Joshua S. 318.03, 318.04,318.05Dimant, Yakov 302.05, 323.03DiMatteo, Tiziana 115.02Ding, Adalbert 323.57Ding, Mingde 111.03DiPompeo, Michael A. 221.04, 410.01Dittmann, Jason 120.15Divin, Andrey 409.02Do Nascimento, José-Dias 322.08,420.04Dobbs, Matt 405.01Doeleman, Sheperd 204.06Domagal-Goldman, Shawn 311.06Domingue, Deborah L. 119.11Dominguez, Alberto 401.04Donahue, Megan 417.09Donovan, Benjamin D 418.02Doppmann, Greg 223.03Dorn-Wallenstein, Trevor 314.02Doschek, George A. 111.05Douglas, Ewan S. 113.09, 122.09,

122.10Douglass, Kelly A 222.09Downes, Tom 411.03Downs, Cooper 218.14, 323.36, 402.01Dragomir, Diana 120.17Draine, Bruce T. 205.01, 220.15Drake, Dereth J 409.05Drake, Jeremy J. 123.43, 319.05Drake, R. Paul 305.04, 413.01, 419.06Dressing, Courtney D. 113.01, 113.03Druckmuller, Miloslav 323.35, 323.57Du, Guohui 218.02Dufour, Reginald J. 121.07, 121.09Dukes, Robert J. 322.16Dumusque, Xavier 301.06Duncan, Michael A 114.02Dunham, Emilie 422.08Dunn, John 409.03Duong, Nhieu 121.16, 121.19, 121.20Dupree, Andrea K. 404.07Dupuy, Trent J. 120.16Durbin, Meredith 421.03Duvall, Thomas L. 117.01Dwarkadas, Vikram 121.18Dwek, Eli 401.01Eccleston, Paul 123.57Edge, Alastair 417.08Edgerton, Melissa 123.61Edmondson, Justin K 123.26Edwards, Phillip 204.05Edwards, Zophia 323.16Eenmäe, Tõnis 421.06Effinger, Robert 311.07Eftekharzadeh, Sarah 221.01Egeland, Ricky 211.05Egorov, Andrey 115.07Ehrenfreund, Pascale 119.06Eidelsberg, Michele 119.04Eisenhamer, Bonnie 320.12Elhoussieny, Ehab E. 221.18Elmegreen, Bruce 223.14Elmegreen, Debra M. 223.14Elsaesser, Andreas 119.06Elvis, Martin 221.13, 222.12, 321.10,410.06Ely, Justin 122.07, 122.08Emery, Logan P 220.11Emilio, Marcelo 218.33Emmanouilides, Constantinos 323.35Emonts, Bjorn 410.04Emslie, A. Gordon 123.22Engle, Scott G. 102.07Errard, Josquin 115.06Erwin, Peter 213.06Espinoza, Nestor 120.14Essey, Warren 407.06Essick, Reed 411.04Esteves, Lisa 416.03Evans, Daniel A. 410.04Evans, Nancy Remage 219.06Evans, Neal J. 317.01Evans, Rebekah M. 323.42Everett, Mark 322.07Everson, Erik 305.01Ewall-Wice, Aaron 318.05Fabbiano, Giuseppina 221.02, 223.12,

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417.03Fabbiano, Giuseppina 222.12Fabricius, M. 213.06Faherty, Jacqueline K. 322.13Falcone, Abraham 122.14, 405.02Falconer, David 212.02, 402.04,408.03Fan, Xiaohui 221.01Fan, Yuhong 211.01D, 212.03, 323.34Fang, Fang 323.34Farber, Ryan 321.04Fardal, Mark A. 213.05Farid, Samaiyah 323.37Farihi, Jay 220.02Farr, Benjamin F. 411.03Farr, Will M 411.03Farrah, Duncan 206.08Farrugia, Charles 323.65Faulkner, Danny R. 219.09, 219.11Faulkner, Danny R 219.10Faussurier, G. 305.02Favia, Andrej 322.14Fayock, Brian 323.11, 323.62Fayolle, Edith 205.04Fazio, Giovanni G. 213.03, 319.07,410.06Federman, Steven Robert 119.04,220.04Feiden, Gregory A. 420.06Feigelson, Eric 105.01Feldman, Allan 415.03Feldman, Uri 106.03Felipe, Tobias 202.06Fender, Rob 204.05Feng, Li 123.29Feng, Lu 318.13Feng, Xueshang 323.31Feng, Yan 409.03Feng, Yu 115.02Ferguson, Henry Closson 417.06Ferland, Gary J. 419.01Field, Tom 413.03Fienberg, Richard Tresch 316.05,320.01Fiksel, Gennady 305.03, 419.06Fillion, Jean-Hugues 119.04, 205.04Finkbeiner, Douglas P. 115.08, 220.05,220.14Finkelstein, Steven L. 417.06Finn, Rose 222.10Finn, Susanna C. 113.09, 122.09Finn, Susanna 122.10Fischbach, Ephraim 211.02Fischer, Christian 418.03Fischer, Debra 122.20Fischer, William J. 220.12Fish, Vincent L. 204.06Fisher, George H. 123.49, 323.18Fisher, Robert 412.03Fitzsimmons, Alan 413.03Fivian, Martin 218.27Fleck, Bernard 323.05Fleischmann, Andreas 119.07Fleishman, Gregory D. 123.12,123.60, 218.45Fleming, Scott W. 120.22, 322.04

Fletcher, Lyndsay 123.39Flowers, Jack 120.22Flurchick, K. M. 219.01Fogarty, Kevin 417.09Foing, Bernard 119.06Fontenla, Juan 302.05, 323.03Fontes, Christopher J 305.02Forbes, Terry G. 212.06Forland, Blake 123.29Forman, William R. 206.04, 222.03,222.05, 222.11, 417.08Forrey, Robert C 413.04Fortney, Jonathan J. 102.02, 120.14,122.12, 201.05Foschini, Luigi 221.15Foster, Adam 121.22, 122.14, 403.05,405.02Foukal, Peter V. 422.01Fox, Lewis 414.06Fox, William 305.03, 323.70, 403.02Fragos, Tassos 223.12Fraine, Jonathan D. 120.14Fraisse, Aurélien A. 417.07Fraknoi, Andrew 306.01, 320.01Frank, Juhan 219.12Freed, Michael 323.44Freed, Michael 104.01, 323.29Freedman, Wendy L. 421.03Freeland, Sam 313.01French, D. A 320.08Frenje, Johan 315.02Friedman, Andrew S. 304.02Froula, Dustin 419.06Fruscione, Antonella 417.03Fuerst, Felix 221.13Fumi, Fabio 418.03Gaches, Brandt A.L. 215.09Gaensicke, Boris T 220.02, 412.01Gaertner, Arnold 405.01Gaintatzis, Pavlos 323.16Galache, Jose Luis 321.10Galera-Rosillo, R. 121.08Gallagher, Peter T 112.03, 123.15,123.16, 123.37Gallicchio, Jason 304.02Galvan-Madrid, Roberto 223.06Galvin, Antoinette B. 323.65Gamer, Lisa 119.07Gandhi, Poshak 410.08Gangadharan, Vigeesh 123.50Gao, Ryan 415.02Garcia, Javier 106.04, 219.17, 221.18Garcia-Alvarez, David 421.01Garcia-Berro, Enríque 412.03Gardner, Jonathan P. 417.06Garmire, Audrey B 222.06Garmire, Gordon 222.06Garnavich, Peter M. 121.15Gary, Dale E. 123.12, 123.32, 123.60,218.45, 323.45Gaskin, Jessica 123.61, 123.62Gasparrini, Dario 410.09Gastaldello, Fabio 417.08Gatuzz, Efrain 106.04Gautam, Abhimat Krishna 405.06Gauthier, Adrienne J. 320.09

Gavilan, Lisseth 119.04Gawiser, Eric J. 417.06Geballe, Thomas R. 322.17Gebhardt, Karl 213.07Gehrels, Neil 311.01, 421.04Geis, Norbert 418.03Gekelman, Walter 305.01, 403.01Gelino, Dawn M. 120.11Geppert, W. 119.07Gerhardt, David 107.02Gerin, Maryvonne 215.01Germaschewski, Kai 305.03, 403.03Gettel, Sara 120.20Gharanfoli, Soheila 318.10Ghavamian, Parviz 412.04Ghez, Andrea M. 213.03Ghezzi, Luan 420.04Giacintucci, Simona 222.03, 417.08Giavalisco, Mauro 417.06Gibson, Zachary J 322.02Gilbert, Holly 111.06, 323.13, 408.04Gilliland, Ronald L. 120.02, 319.04Gingerich, Owen 306.05Ginsburg, Idan 411.01Ginsburg, Idan 120.21Giovanelli, Riccardo 222.01, 318.08Girouard, Forrest 120.06Gizis, John 322.13Glesener, Lindsay 104.06, 123.02,123.38, 123.62, 123.64Godfrey, L. E 221.10Goes, C. W 223.11Golden-Marx, Jesse B. 121.02Goldfinger, David 122.15Goldsmith, Paul 215.01Golovkin, I. 305.02Golub, Leon 123.56, 323.20, 323.47Gomez, Daniel O. 303.02Gomez, Sebastian 219.20Gonzales-Solares, Eduardo 206.08Goode, Philip R. 112.01, 323.01,323.08Gopalswamy, N. 303.06Gorczyca, Thomas 106.04Gordon, Karl D. 220.01, 220.03Gosmeyer, Catherine 122.03Goss, Miller 223.06Gou, Tingyu 111.04Graff, Philip 411.03Grant, Catherine E. 122.13Graus, Andrew S 121.02Greathouse, Thomas K. 418.04Green, Gregory 220.05Green, Richard F. 316.05Grefenstette, Brian 123.64Gregory, Kyle 123.61Greiner, Jochen 120.21, 319.03Greiss, Sandra 219.18Griego, Ben 219.01Griffin, Douglas 123.57Grinberg, Victoria 219.17Grindlay, Jonathan E. 110.06, 118.01,122.16, 321.11, 410.05Groenenboom, Gerrit C 413.04Grogin, Norman A. 122.01, 417.06,418.01

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Gronwall, Caryl 417.06Grundy, William M. 214.03Guennou, Chloe 323.53Guenther, Hans Moritz 419.05Guidoni, Silvina 104.05, 403.06Guinan, Edward F. 102.07Gunning, Heather C. 122.04Guo, Fan 123.40Guo, Yang 111.03Gupta, Harshal 119.08Gurman, Joseph B. 218.41Gurton, Suzanne 316.02, 320.01Gusain, Sanjay 123.54Gutermuth, Robert A. 220.12, 223.01Guth, Alan 304.02Gutierrez, Joseph V 320.08Guzman, Andres 215.03, 220.13Guzman Fernandez, Andres 223.01Haas, Patrick 123.57Habbal, Shadia R. 323.35, 323.57Hack, Warren J. 122.02Haden, Carol 320.11Haggard, Daryl 213.01Hahn, Michael 323.53, 408.06Hainline, Kevin 410.01Hall, Kendall Paige 220.10Hallenbeck, Gregory 222.01Hallinan, Gregg 107.04Hamer, Steven 417.08Hammel, Heidi B. 210.02Hammer, Derek 122.03Hammer, Michael 123.41Han, Xianming L. 417.05Hanish, Daniel 417.06Hanna, Chad 411.03Hannah, Iain 123.64, 218.10Hansen, S. B 305.02Hanson, Chris S 112.04Hanson, Elizabeth 303.01Hanson, Margaret M. 314.01Hansteen, Viggo 313.02, 313.05Hao, Lei 119.10Hara, Hirohisa 104.06Harding, Alice Kust 121.10, 121.11Harker, Brian 123.34Harlow, George 119.11Harper, Graham M 418.04Harris, D. E. 221.10Harris, Hugh C. 322.13Harrison, Fiona 122.16, 221.12, 221.13Harrison, Samuel 415.02Harrison, Thomas E. 420.06Hartmann, Dieter 421.04Harvey, J. W. 123.21, 123.27Hasan, Hashima 316.03Hasan, Imran 410.03Haster, Carl-Johan 411.03Hathaway, David H. 103.01D, 218.09Haynes, Martha P. 222.01, 222.10,318.08Hayward, Christopher C. 215.07,222.16He, Jiao 119.09, 205.03Heays, Alan 119.04Heckman, Timothy M. 410.08Hedman, Matthew M. 122.12

Heerikhuisen, Jacob 323.62Heinz, Sebastian 222.03, 307.01Heinzel, Petr 123.39Henden, Arne A. 110.04, 207.01Hendrick, Sean Patrick 412.04Henney, Carl John 323.23, 323.36Henning, Thomas 220.12Henry, Richard B. C. 121.07, 121.08,121.09, 121.14Henry, Todd J. 120.26, 122.20Hensley, Brandon 220.15Hensley, Kerry G. 121.08, 121.14Herbst, William 223.04Hermes, JJ 412.01Hernandez, Svea 122.07, 122.08Hernquist, Lars E. 222.16Herter, Terry L. 213.02D, 223.01Hertzberg, Mark P 423.01Hess, Phillip 218.28Hess Webber, Shea A. 323.55Hessels, Jason 121.12Hewett, Russel 218.39Hewitt, Jacqueline N. 318.05, 318.06,318.13Hickox, Ryan C. 206.02, 320.09,410.01Hicks, Brian 113.09, 120.13, 122.10Higgins, Paul A. 112.03, 123.16Hill, Frank 123.54, 218.01, 218.21Hill, Robert L. 219.10Hill, Tracey 223.02Hillier, Andrew 212.01Hintz, Eric G. 322.18Hirsch, Brian 311.07Hirst, Dalton 320.07Ho, Shirley 410.07Hock, Rachel 123.05Hodge, Philip 122.07, 122.08Hoeksema, J. Todd 123.52Hoeksema, Jon Todd 103.06, 323.64Hoffman, Jennifer L. 121.16Holberg, Jay B. 219.16, 319.04Holbrook, Jarita 203.05Holman, Gordon D. 104.04, 123.33Holman, Matthew J. 314.06Holmbeck, Erika 419.07Homan, Daniel C. 221.15Hong, JaeSub 122.16, 321.11Hönle, Rainer 418.03Hopkins, Philip F. 215.06Hoq, Sadia 220.06, 220.08Hora, Joseph L. 213.03, 223.01,223.07Hornig, Gunnar 402.06Horst, Chuck 121.16, 121.19, 121.20Horst, Sarah 214.01Hourcle, Joseph 218.40, 218.48,405.08Hovatta, Talvikki 221.09, 221.15Howard, Andrew 210.03Howard, Tim A. 218.26, 323.63,408.01Howell, Steve B. 322.07Howes, Gregory G. 409.05Hoyle, Fiona 318.08Hu, Qiang 218.12, 323.31

Hu, Suxing 305.03Huang, Jiasheng 213.03, 410.06Huang, Shan 222.01Huber, Daniel 102.03, 113.04, 120.16Hudson, Hugh S. 123.11, 123.31,123.49, 123.64, 218.10, 218.27,323.49Huenemoerder, David 421.01Huffenberger, Kevin 115.05Hughes, A. M 322.21Hughes, Philip A. 221.09Hughitt, V. Keith 218.44Huk, Leah N. 121.16Hull, Anthony B. 122.21Hulsebus, Alan 113.08Hung, Chao-Ling 206.07, 215.07Hunniford, Adam 413.03Hunt, Leslie K 222.01Hurford, Gordon J. 123.60, 123.64Hurlburt, Neal E. 313.01Hurst, Anna 320.01Hutchinson, Trevor 409.03Hutter, Donald J. 404.05Hynes, Robert I. 219.18, 420.02Ibata, Rodrigo 319.01Ichimoto, Kiyoshi 123.63Iglesias, C. A 305.02Ignace, Richard 314.03, 404.06Ilonidis, Stathis 202.02Imada, Shinsuke 323.25Inamdar, Niraj K 321.11Ingalls, James 213.03Inglis, Andrew 123.08, 218.39,323.13, 323.21, 323.43Innes, Davina 123.18, 323.06, 323.09Inoue, Yoshiyuki 407.02Intrator, Thomas 409.03Ireland, Jack 123.08, 218.39, 218.44,323.21, 323.43Ireland, Michael 120.16Irwin, Jonathan 120.15, 404.03Irwin, Michael 319.01Isella, Andrea 322.22Isler, Jedidah 410.03Ivezic, Zeljko 319.01Jackiewicz, Jason 123.50, 218.03Jackson, Brian K. 416.01Jackson, William M. 114.03Jaeckel, Felix T 419.03Jaeggli, Sarah A. 123.44, 302.01,323.06Jahan, Nabila 121.15Jain, Kiran 218.21Jameson, Katherine 215.04Janes, Kenneth 102.09Jang, Bi-Ho 323.08Jang, Soojeong 218.34, 218.35Janish, Ryan 213.07Jao, Wei-Chun 120.26Jarvis, Matt 206.08Javornik, Brenda 218.07Jayaraman, Arun 318.11Jayawardhana, Ray 416.03Jedrzejewski, Robert I. 122.07, 122.08Jenkins, Jere 211.02Jenkins, Jon Michael 113.04, 120.01,

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120.03, 120.04, 120.05, 120.06,120.08, 120.09Jensen, Eric L. N. 219.08Jensen, Joseph B. 322.02Jernigan, J. Garrett 107.06, 122.23Jessberger, Elmar K 119.06Jha, Saurabh 121.15Ji, Haisheng 123.29, 218.20Ji, Hantao 323.70, 403.02Ji, Li 403.05Ji, Suoqing 412.03Ji, Tuo 417.05Jia, Jianjun 410.08Jiang, Chaowei 323.31Jibben, Patricia R. 323.52Jing, Ju 123.04, 414.01Johnson, Beth 222.07Johnson, Christian I. 319.01, 319.02Johnson, Christopher Bradley 219.18Johnson, John A. 102.08, 120.12,210.03, 314.04, 420.04Johnson, Michael 204.06Johnson, Ryan 222.02Joiner, David A. 120.17Joner, Michael D. 219.08, 221.07,322.18Jones, Amy 405.03DJones, Christine 206.04, 222.05,222.11Jones, Christine 206.03, 222.02,222.03Jones, Dayton L. 107.03Jones, Michael 222.01Jones, William C. 417.07Jonker, Peter 219.18Jordan, Andres 120.14Jordan, Patrick 123.57Jorgensen, Anders M. 404.05Jorstad, Svetlana G. 221.08, 221.09,221.14, 221.19, 410.02Joshi, Manasvita 410.02Joyce, Meridith 420.06Joyce, Richard R. 121.15Juda, Michael 321.03Judge, Philip G. 123.09, 211.05,323.24, 422.04Kadam, Kundan 219.12Kadler, Matthias 221.15Kahler, Stephen W. 123.18, 323.58Kaiser, David I 304.02Kalapotharakos, Constantinos 121.10,121.11Kallman, Timothy R. 106.04, 221.18,403.05Kaltenegger, Lisa 102.01Kanbur, Shashi 219.07Kane, Stephen R. 120.11, 120.17Kang, Minhee 223.08Kang, Yong Beom 223.13Kankelborg, Charles 123.55, 218.49,414.06Kaplan, David L.A. 121.12Karas, Vladimir 204.02Karkare, Kirit S 415.01, 415.02Karna, Nishu 323.55Karovska, Margarita 219.15

Karpen, Judith T. 104.05, 111.06,323.51, 403.03, 403.06, 408.04Kasdin, N. Jeremy 311.06Kashlinsky, Alexander 407.05Kashyap, Rahul 412.03Kashyap, Vinay 123.43Kasliwal, Vishal P. 221.06Katsavounidis, Erotokritos 411.04Kausch, Wolfgang 405.03DKautsch, Stefan J. 320.06Kawaler, Steven D. 406.01Kay, Christina 120.24, 303.05Kazachenko, Maria D. 123.49Kazanas, Demosthenes 121.10, 121.11Keck, Mason 221.13Kelly, Brandon C. 410.05Kentrianakis, Michael 323.16Keto, Eric R. 223.06Khandai, Nishikanta 115.02Khandrika, Harish G. 121.16, 121.19,121.20Khazanov, Igor 402.04Kiessling, Alina 418.05Kilcrease, D. P 305.02Kilgard, Roy E. 314.02Kim, Dong-Woo 221.02, 222.12,223.12, 417.03Kim, Ji Seok 421.02Kim, Jongsoo 220.17Kim, Kap-Sung 218.36Kim, Sooyoung 223.13Kimberk, Robert S 415.01, 415.02Kimeswenger, Stefan 405.03DKipping, David M. 102.03, 120.25Kirk, Michael S. 218.47Kirkpatrick, Allison 222.16Kirshner, Robert P. 412.07Kiss, Laszlo 219.06Kissel, Steven E 321.11Kissil, Andrew 311.07Kitiashvili, Irina 103.04, 323.02,404.02, 422.07Kiyokane, Kazuhiro 223.02Kiziltan, Bülent 204.08, 306.03Klaus, Todd C. 120.06Klein, Randolf 418.03Klein, Sallee 413.01Kleint, Lucia 123.14, 313.06, 409.06Klessen, Ralf 223.06Kletzing, Craig A 409.05Kliem, Bernhard 212.06, 312.02Klimchuk, James A. 123.24, 123.25,302.06, 312.04, 323.15, 323.42Klimenko, Sergey 411.04Knee, Lewis 223.02Kneib, Jean-Paul 410.07Kneip, Raymond 421.06Knizhnik, Kalman J. 111.06, 408.02Knox, Javon M 212.02Ko, Yuan-Kuen 323.66Kobayashi, Ken 323.11Kobelski, Adam 312.01DKoch, Andreas 319.01Kodama, Tadayuki 223.13Koekemoer, Anton M. 417.06Koenig, Xavier 223.07

Koenke, Samuel 219.10Koester, Detlev 220.02Kohnert, Rick 107.02Kolodziejczak, Jeffery J 120.07Komm, Rudolf W 218.21Komm, Rudolf 218.01Kong, Xiangliang 123.40Kontar, Eduard 123.12, 123.22Koopmann, Rebecca A. 222.10Kopacek, Ondrej 204.02Kopp, Greg 123.27Korhonen, Heidi 322.11Kornbleuth, Marc 321.03Korpela, Eric J. 405.06Korzennik, Sylvain G. 218.13Kosiarek, Molly 422.08Kosovichev, Alexander G. 103.04,104.03, 123.10, 123.45, 218.05,218.11, 323.01Kosowsky, Michael 204.06, 219.23,219.24Koss, Michael 206.07Kovac, John M 415.01, 415.02Kovacs, J. Paul 405.01Kozarev, Kamen A. 123.41Kozhurina-Platais, Vera 122.02Kozlovsky, Benz-zion 123.03Krabbe, Alfred 418.03Kraemer, Kathleen E. 223.11Kraft, Ralph P. 206.04, 222.03, 222.05Kramar, Maxim 323.30Krantz, C. 119.07Kraus, Adam L. 120.16Kreckel, H. 119.07Krennrich, Frank 401.02Kress, Monika 120.17Kring, James 420.03Kring, James 219.09Krist, John E. 311.07Krolewski, Alex 415.01Krucker, Sam 104.06, 123.11, 123.31,123.38, 123.62, 123.64Krumholz, Mark R. 220.03Kucera, Therese A. 111.06, 408.04Kuchar, Thomas Andrew 218.04Kuchner, Marc J. 311.06Kuhn, Jeffrey Richard 218.33Kulas, Kristin 418.04Kulkarni, Varsha P. 318.10Kullberg, Evan 102.07Kunder, Andrea 319.01, 319.02Kunneriath, Devaky 204.02Kuntz, K. D. 314.02Kuranz, Carolyn C. 413.01, 419.06Kurczynski, Peter 417.06Kurinsky, Noah 222.17Kuroda, Natsuha 123.32Kurono, Yasutaka 223.02Kusano, Kanya 212.05Kwak, Kyujin 220.17Kwitter, Karen B. 121.07, 121.08,121.09, 121.14, 219.05Kwon, Ryun Young 218.06La Parola, Valentina 421.04Lacerda, Pedro 413.03Lackner, Claire 318.11

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Lacy, John H. 213.01Lacy, Mark 206.08Lagadec, E. 223.11Lai, Shih-Ping 404.08LaMarr, Beverly 122.13LaMassa, Stephanie M. 410.08Lamb, Joel B 121.02Lambert, David L. 220.04Landavazo, Matthew 404.05Landi, Enrico 312.04, 323.39Lang, Cornelia C. 417.01Lang, Dustin 410.07Lang, Jared 311.07Lanz, Lauranne 215.07, 410.04Lapenta, Giovanni 409.02Larionov, Valeri M 221.19Larsen, Kristine 320.03, 320.13Larson, Kirsten 206.07Laskar, Tanmoy 421.08Latham, David W. 102.04, 102.05,113.02, 322.01Lau, Ryan M. 213.02D, 223.01Lauer, Jennifer 417.03Lauer, Tod R. 213.07Laurent, Pierre 221.01Law, Casey J. 204.07Law-Smith, Jamie 415.02Lawrence, Earl 204.07Lawrence, Eric 323.70Lawton, Brandon 316.02Lawton, Brandon L. 220.01, 320.12Lazio, Joseph 204.07Lazio, T. Joseph W 107.04Le Goff, Jean-Marc 221.01Leake, James E. 312.02Leake, James Edward 103.03, 302.03Leamon, Robert 323.38, 422.05Lebofsky, Matt 405.06Lee, Dongwook 412.03LEE, Harim 218.34, 218.35Lee, Hyun Taek 220.17Lee, Hyun-chul 322.02Lee, Hyunju 415.03Lee, Jea-Ok 218.35Lee, Jin-Yi 123.42, 218.36Lee, Julia C. 204.05Lee, Kyoung-Soo 417.06Lee, Nicholas 206.07Lee, Young-Wook 223.13Lee, Youngung 419.02Leenaarts, Jorrit 323.05Leibacher, John W. 218.17Leka, K D. 112.03, 218.15Lemaire, Jean Louis 119.04, 205.02Leonard, Douglas C. 121.16, 121.19,121.20Lepine, Sebastien 120.21, 319.03,411.01Lepri, Susan T. 323.66Leroy, Adam K. 215.04Leske, Richard A 323.68Levay, Karen 322.04Levay, Zoltan G. 417.06Leventhal, Marvin 121.21Levi, Amit 120.23Levine, Alan M. 113.03

Levine, Stephen 122.19Lewis, John A. 121.17Lewis, Nikole 102.02, 120.14, 122.09,201.05Lezcano, Andrew 322.06Li, Aigen 119.10, 413.02Li, Chikang 419.06Li, Gang 123.40Li, Gongjie 102.08Li, Jie 120.01, 120.06Li, Xinlin 107.02Li, Yan 218.16, 323.68, 323.69Li, Yanxia 206.07Li, Yaqiong 419.03Li, Ying 111.03Li, Yuexing 215.08Liebst, Kelley 215.05Liedtke, Simon 218.39Liggins, Florence 119.02Lim, Jeremy 417.08Lin, Haosheng 123.58, 302.04Lindsay, Kevin 122.07, 122.08Linker, Jon A. 212.04, 218.08, 312.03,323.36, 323.40, 323.41Linnartz, Harold 205.04Linsky, Jeffrey 102.01Linton, Mark 103.03, 212.05, 302.03,312.02Lionello, Roberto 312.03, 323.36,323.40, 323.41Lipartito, Isabel 222.14Lisman, Doug 311.06Lister, Matthew L. 221.15, 417.04Little, John 421.02Liu, Adrian 318.03Liu, Chang 123.04, 414.01Liu, Hauyu B 215.02Liu, Jifeng 319.03Liu, Kai 111.04Liu, Michael C. 322.13Liu, Rui 111.04, 414.01Liu, Wei 212.01, 218.14, 313.03,409.06Liu, Wei 414.04Liu, Wenjuan 123.13Liu, WenJuan 417.05Liu, Yang 103.06, 123.46, 323.38,323.64Liu, Zhong 414.01Livingston, William 112.02Lockhart, Kelly 206.07Loisel, G. 305.02Long, Knox S. 412.04Longcope, Dana 111.02, 123.13,123.24, 123.25, 323.29, 323.38,323.44Looney, Leslie 418.03Lopez, Isaac 420.02Lopez-Morales, Mercedes 120.14Lorén-Aguilar, Pablo 412.03Lorimer, Duncan 121.12Los, Edward 110.06, 410.05Low, Boon Chye 212.01Lowder, Chris 323.38Lowenthal, James D. 222.14Lowrance, Patrick 121.03

Lu, Rusen 204.06Lu, Xing 215.02Lu, Zhou 114.03Lucas, Robert 323.16Ludovici, Dominic 417.01Lugaz, Noe 212.05Luhmann, Janet 218.16, 323.68,323.69Lukin, Vyacheslav 103.03, 112.06,323.07, 323.70Luna, Manuel 111.06Lunnan, Ragnhild 121.13, 421.08Luo, Bin 223.12Lynch, Benjamin J. 123.26, 218.16Lynch, Ryan 121.12Lynch, Ryan 411.05Lyons, James R. 119.04Ma, Chung-Pei 213.07Mac Low, Mordecai-Mark 223.06Maccarone, Tom 219.18MacDonald, Nicholas R. 221.08,410.02MacFarlane, Joseph J. 305.02MacGregor, Meredith A. 322.21Machalek, Pavel 120.22Macintosh, Bruce 301.02Mack, Claude E. 102.06Mack, Jennifer 122.03Mackay, Duncan 112.05MacKenty, John W. 122.04, 122.06Macneice, Peter J. 323.26MacPherson, Emily 410.03Madejski, Grzegorz Maria 221.13Madore, Barry F. 421.03Madsen, Chad Allen 302.05, 323.03Maji, Moupiya 215.08Malamud, Guy 413.01Malanushenko, Anna 218.18, 321.02,323.19Malmrose, Michael P. 221.14Malphrus, Benjamin K. 122.23Mancini, Roberto 305.02Mandel, Ilya 411.03Mandelbaum, Rachel 115.02, 206.01,318.11, 423.04Manjunath, Ramya 122.18Mann, Andrew 120.16, 404.04Manning, James 306.01Manning, Jim 316.02Mansour, Nagi N 103.04Manuel, Mario 305.04Mao, Peter H. 122.16Maraston, Claudia 206.08Marble, Andrew R. 218.31Marcello, Dominic 219.12Marchesini, Danilo 206.08, 222.15Marchetti, Lucia 206.08Marcy, Geoffrey W. 210.03Marengo, Massimo 113.08, 215.03Margutti, Raffaella 421.08Marinucci, Andrea 221.12Markatou, Evangelia Anna 422.08Markevitch, Maxim L. 222.03Markidis, Stefano 409.02Markwardt, Craig 421.04Marley, Mark S. 102.02, 201.05,

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210.02, 311.07Marrone, Daniel P. 204.06Marsan, Zehra Cemile 222.15Marscher, Alan P. 221.08, 221.09,221.14, 221.19, 410.02Marsh, Andrew 123.02, 123.64Marshall, Sunette Sophia 320.02Martel, Jason 113.09, 122.09, 122.10Martens, Petrus C. 211.03, 211.05,218.29Martignoni, Massimiliano 421.06Martin, John C. 421.06Martin, Sara F. 414.03Martin, Suzanne 311.06Martinez, Rafael 215.03Martinez Oliveros, Juan Carlos 123.11,123.28, 123.31, 123.38, 323.67Martinez Pillet, Valentin 112.02Martinez-Galarza, Juan Rafael 215.07,220.13Martinez-Sykora, Juan 313.06Marzari, Francesco 120.18Mason, Paul A. 219.20, 420.02Massa, Derck 122.07, 122.08Massey, Angela P 404.04Massey, Richard 417.07Masson, Sophie 218.16, 218.37Masters, Karen 222.01Masterson, Rebecca 321.11Matheson, Thomas 121.15, 319.04Mathews, William G. 417.08Mathioudakis, Mihalis 123.39Matsushita, Satoki 222.01Matt, Giorgio 221.12, 221.13Matthaeus, Bill 323.63Matthews, Jaymie 219.06Matthews, Lynn D. 121.04Matthews, Morgan 420.06Mattmann, Chris 204.07Matzke, David 219.02Mauduit, Jean-Claude 206.08Mays, Leila 323.13, 323.68, 323.69Mayyasi-Matta, Majd Mayyasi 321.05Mazzalay, X. 213.06McArthur, Barbara 420.06McAteer, James 323.23, 323.43Mcateer, Robert TJ 323.21McBride, Cameron 221.01, 410.07McCammon, Dan 419.03McCauley, Patrick 218.22, 218.30McCauley, Patrick I 218.20, 323.14,402.01McCauliff, Sean D 120.06McCauliff, Sean 120.09McClintock, Jeffrey E. 219.17McCollough, Michael L 219.22McCollough, Mike 417.03McComas, Dave 408.01McConnell, Nicholas J. 213.07McCullough , Bob 413.03McCullough, Peter R. 120.22McDowell, Jonathan C. 221.13McElwain, Michael W. 311.07McEntaffer, Randall L. 122.14, 405.02,418.02McGreer, Ian D. 410.07

McIntosh, Melissa 121.17McIntosh, Scott W. 218.18, 313.02,313.04, 422.05McKee, Christopher F. 220.03McKelvey, Mark 418.04McKenzie, David Eugene 104.01,111.05, 312.01D, 323.29, 323.44McKillop, Sean 218.30, 303.01McKillop, Sean 313.06McKinney, Jonathan C. 204.01McLaughlin, Maura 121.12McLeod, Kim K. 321.10McMurray, Robert 418.04McNeil, S. 122.23McTiernan, James 123.07, 123.60McWilliam, Andrew 420.05, 420.06Mead, Lawrence R 115.03Meadows, Victoria 311.07Medvedev, Mikhail 409.01Megeath, S. Thomas 220.12Megeath, S. Tom 223.01Meibom, Soren 123.43, 322.05Meinke, Bonnie K. 306.01Meisner, Aaron M. 220.14Meixner, Margaret 215.04, 217.01Melis, Carl 419.09Mendelsohn, Benjamin 320.07Mendillo, Christopher Bernard 113.09,122.09, 122.10Mendillo, Michael 306.06Mendoza, Claudio 106.04, 119.03Meng, Xiao-Li 105.03Mesinger, Andrei 318.05Messias, Hugo 206.08Mewaldt, Richard A. 123.64Meyer, Karen 323.10Meyer, Karen 112.05Meyer, Leo 213.03Meyer, Manuel Enrico 407.04Michael, Scott 319.01, 319.02Michaut, Xavier 205.04Michener, Scott 102.07Miesch, Mark S. 211.01D, 211.04Mikic, Zoran 212.04, 218.08, 312.02,312.03, 323.36, 323.40, 323.41Miller, Eric D. 122.13Miller, George Franklin 110.06, 410.05Miller, John 411.02Miller, Kenneth A. 119.05, 119.11Miller, Kenneth A. 119.05, 119.11Miller, Sarah 418.05Miller, Timothy R. 121.07Milligan, Ryan O. 123.15Million, Chase 322.04Milne, Peter 121.16Milone, Eugene F. 420.01Mineo, Stefano 223.12Mininni, Pablo D 303.02Miralda-Escude, Jordi 221.01Miralles, Mari Paz 218.30, 323.56Misenti, Victoria 122.20Mishra, Ajay 413.02Misselt, Karl A. 220.01Miyasaka, Hiromasa 122.16Mizusawa, Trisha 219.16Mohanty, Subhanjoy 102.01

Mok, Yung 312.03, 323.40, 323.41Monier, Eric M. 423.02Monson, Andrew 421.03Monsrud, Ashley 223.06Montet, Benjamin 210.03, 314.04Montez, Rodolfo 121.05Montgomery, Jordan 220.06, 222.04Montiel, Edward J. 322.17Moon, Yong-Jae 123.18, 123.42,218.34, 218.35, 218.36Moore, Benjamin John 421.05Moore, Ronald L. 212.02, 402.04,408.03, 409.04Moorman, Crystal 318.08Morgan, Doug 417.03Morgan, Dylan P. 322.12Morgan, Huw 323.57Morgan, Kelsey 419.03Morris, Mark 213.02D, 213.03Morris, Patrick W. 119.08Morris, Robert L. 120.08Morton, Richard 312.06Morton, Tim 113.03Moskovitz, Nicholas 321.09Mossman, Amy 417.03Motl, Patrick M. 219.12Moustakas, John 121.19, 417.09Mozurkewich, David 404.05Mueller, Daniel 218.44Mueller, Hans R. 219.13Muglach, Karin 111.06, 323.33,323.66Muirhead, Philip Steven 122.12Mukadam, Anjum S. 412.01Mullally, Fergal 113.04Mumford, Stuart 218.39Munoz-Jaramillo, Andres 211.03,218.29Muntean, Elena Andra 413.03Murase, Kohta 407.03Murgia, Matteo 222.03Murphy, Nicholas Arnold 218.30,323.07, 323.70, 414.02Murphy, Ronald 111.01, 123.03Murray, Stephen S. 222.02Murray-Clay, Ruth 210.01Myers, Adam D. 221.01, 221.04,221.05, 410.01, 410.07Myers, Clayton E 403.02Myers, Philip C. 220.12Na, Hyeonock 218.34Na, Hyeonock 218.35Naduvalath, Balakrishnan 413.04Nagayama, T. 305.02Nagy, Zsofia 119.08Nah, Jakyung 323.08Nahar, S. N 305.02Naoz, Smadar 102.08Narayan, Gautham 115.01D, 319.04Narayan, Ramesh 204.01, 204.04NASA SMD Astrophysics E/POCommunity, The 316.02Nash, T. J 305.02Nave, Gillian 119.02Neben, Abraham Richard 318.06Neilsen, Joseph 204.05

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Neilson, Hilding 314.03Nejat, Cyrus 122.22Nejat, Najmeh (Setareh) 122.22Nejat, Narsis 122.22Nelan, Edmund P. 420.06Nelemans, Gijs 219.18Nelson, Nicholas J. 211.04Netterfield, Calvin Barth 417.07Newman, Jeffrey 410.07Newman, Kyle 404.05Newton, Elisabeth R. 120.15, 121.17,320.05, 404.03Ng, Cheuk Y 114.03Nguyen, Duy Cuong 120.22Nguyen, My L. 221.05Nichols, Joy S. 421.01Nicholson, Philip D. 122.12Nielson, Kevin D 409.05Niemann, Christoph 305.01Nilson, Philip 305.03Nissen, Joel 311.07Nita, Gelu M. 123.12, 123.60, 218.45Nitta, Nariaki 303.04Nittler, Larry R. 123.23, 214.02Nofi, Larissa 219.21Noll, Stefan 405.03DNonaka, Andrew 121.01Nordlund, Aake 103.02Norris, John E. 102.06Norris, Mark A. 222.08Norton, Aimee Ann 323.64Novotny, Oldrich 119.07Nowak, M. 213.06Noyes, Robert W. 203.01Nulsen, Paul 206.06, 222.05Nyman, Lars-Ake 223.02O'Callaghan, David 112.03O'Connor, Aodh 119.05O'Connor, Brian 123.61O'Dell, C. R. 419.01O'Flannagain, Aidan M 123.37O'Malley, Erin M. 420.05O'Neill, John Francis 123.59O'Sullivan, E. J 417.03Oberg, Karin I. 205.04Odden, Caroline 421.02Odstrcil, Dusan 323.69Oey, M. S. 121.02Offner, Stella 215.09Ofman, Leon 218.14, 323.13, 323.48,323.54, 408.05Ogle, Patrick M. 410.04Ohyama, Youichi 417.08Oktem, Figen S 123.59Oliveira, Cristina M. 122.07, 122.08Olshevsky, Vyacheslav 409.02Olson, Roberta J. M. 203.06Olszewski, Edward W. 319.04Omodei, Nicola 414.04Opher, Merav 120.24, 303.05Oppenheim, Meers 302.05, 323.03Oprescu, Antonia 120.21, 321.11,411.01Oram, Kathleen 120.13Orban, Chris 305.02Orvedahl, Ryan 121.01

Oseas, Jeffrey 311.07Osip, David J. 120.14Oswalt, Terry D. 219.16Owen, Aaron 122.23Paggi, Alessandro 221.02, 222.12Palanque-Delabrouille, Nathalie221.01, 410.07Palo, Scott 107.02Pan, Danny 318.08Panesar, Navdeep 321.01Pankow, Chris 411.03Pankratius, Victor 105.02Pannuti, Thomas 421.07Pariat, Etienne 303.01Paris, Isabelle 410.07Park, Hyungmin 323.08Park, Jinhye 123.18Park, Young-Deuk 323.08Parrish, Michael 112.03Parsons, Aaron 318.03Parsotan, Tyler 322.19Pasachoff, Jay M. 203.06, 323.16Patel, Nimesh A. 415.01Patel, Rishi N 415.01Paterno-Mahler, Rachel 206.05,222.02Patsourakos, Spiros 212.06, 323.28Patterson, Richard J. 420.06Pavel, Michael D. 220.06Pearson, John 119.08Peeters, Zan 119.06Pellegrini, Silvia 222.12Penev, Kaloyan 416.01Penn, Matthew J. 112.01, 112.02Penna, Robert F. 204.04Penny, Matthew 311.03Penton, Steven V. 122.07, 122.08Pepper, Joshua 219.08Percival, William 410.07Pereira, Tiago M.D. 313.02, 323.05Pereyra, Nicolas Antonio 221.03Perez, Laura M. 322.22Perez-Suarez, David 112.03, 218.39Pesce-Rollins, Melissa 414.04Pesnell, W. Dean 323.59Pesnell, William D 323.55, 422.03Peter, Hardi 313.04Peters, Thomas 223.06Peticolas, Laura 316.01Petitjean, Patrick 221.01, 410.07Petre, Natalia 419.03Petre, Robert 122.14, 405.02Petrie, Gordon 123.27, 123.28Petrosian, Vahe 104.02, 409.06,412.06, 414.04Pevtsov, Alexei A. 123.28, 123.34,218.31, 323.26Pewett, Tiffany 120.26Pforr, Janine 206.08Philippe, Laurent 205.04Phillips, Kenneth 123.23Phung, Chau 320.06Pickering, Juliet C 119.02Pierpaoli, Elena 115.07Pilachowski, Catherine A. 319.01,319.02

Pinkerton, Stephen 218.23Pinsonneault, Marc H. 305.02Pipher, Judith 220.12Pivovaroff, Michael 123.64Plambeck, Richard L. 204.06Plavchan, Peter 120.10, 120.12Plovanic, Jacob 414.06Plowman, Joseph 323.24Plucinsky, Paul P. 319.05Plummer, Thomas 123.57Pober, Jonathan 318.03Podolak, Morris 120.23Poduval, Bala 323.60Poglitsch, Albrecht 418.03Pokhrel, Riwaj 220.12Polidan, Ronald S. 122.10Polishook, David 321.09Pomeroy, J. Richard R 320.02Pompea, Stephen M. 316.05Ponder, Kara A 121.15Ponti, Gabriele 204.05Pontin, David 323.46, 402.06Pope, Alexandra 222.16Postman, Marc 417.09Powell, Johnny 220.11Pradhan, Anil Kumar 305.02Prather, Edward E. 320.07Preston, Heather L. 322.06Price, Larry 411.03Primini, Francis A. 120.21, 319.03,411.01Proffitt, Charles R. 122.07, 122.08Protopapa, Silvia 214.03Provornikova, Elena 323.48, 323.54,408.05Provornikova, Elena 323.13Ptak, Andrew 122.14, 405.02, 410.08Qiu, Jiong 123.09, 123.13, 123.24,123.25, 123.36, 218.12, 218.32,323.38Quillen, Alice C. 417.02Quinn, Samuel Noah 120.19Quintana, Elisa V. 113.06, 120.01,120.06Raab, Walfried 418.03Rabin, Douglas M. 312.04, 323.39Rachubo, Alisa 121.16, 121.19,121.20Rackham, Benjamin 120.14Rafelski, Marc 417.06Raghavan, Deepak 120.19Ramakrishnan, Venkatessh 221.09Ramirez, Solange 120.10Randall, Scott W. 206.04, 222.02,222.03, 222.05Ransom, Scott M. 121.12Rao, Sandhya 423.02Rasio, Frederic A. 102.08Rasmussen, Eric J 219.02Ravindra, B. 218.21Ravindranath, Swara 417.06Raymond, John C. 123.41, 218.36,323.07, 402.01, 412.04, 414.02Readhead, Anthony C. S. 221.15Reale, Fabio 313.05Reardon, Kevin P. 203.04, 218.43,

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302.01, 323.04Rebell, Felix 418.03Reddy, Krishna 122.18Redfield, Seth 220.02Reed, Phillip A. 219.08, 219.14Rees, Richard F. 223.09Reeves, Kathy 218.08, 218.20, 218.36,313.06, 323.14, 323.52Reginald, Nelson Leslie 123.57Reid, Aaron 302.01Reimer, Anita 401.04Reinard, Alysha 218.01Reipurth, Bo 419.04Remillard, Ronald A. 219.17Rempel, Matthias 218.03Rempel, Matthias D. 202.04, 218.07Rest, Armin 110.02, 121.15, 319.04Restaino, Sergio R 404.05Rey, Soo-Chang 223.13Reyes, Luis C. 401.04Reynolds, Stephen P. 412.04Rhee, Joseph 419.09Rhodes, Edward J. 218.23Rhodes, Jason 417.07, 418.05Ricci, Luca 322.22Ricco, Antonio 119.06Rice, Thomas 419.04Rich, Jeffrey 421.03Rich, Robert Michael 319.01, 319.02Richards, Gordon T. 221.06Richards, Joseph L 221.15Richards, Joseph 405.05Richardson, Dean Leon 421.05Richmond, Michael W. 221.17Richter, Matthew 418.04Ricker, George R. 113.02, 113.03Riedel, Adric R. 120.26Riley, Pete 323.36Rimmele, Thomas R. 218.43Ringermacher, Harry I. 115.03Ringwald, Fred 219.03, 220.10Risaliti, Guido 221.12, 221.13Ritchey, Adam M. 220.04Roach-Barrette, W. 122.23Roberge, Aki 311.06Robert, François 119.06Roberts, D. A 213.01Roberts, David H. 219.23, 219.24,221.16Robin, Annie 319.01Robins, Derek 415.02Robinson, Andrew 221.17Robinson, Edward L. 219.20, 420.02Rochais, Thomas 221.04Rochau, G. A 305.02Roche, Joseph 112.03Rodgers, Bernadette 223.03Rodler, Florian 120.14Rodriguez, Justin 120.26Rodriguez, Marcello 123.61Roebuck, Eric John 222.16Roediger, Elke 206.04Rogers, Anthony 322.04Roman-Duval, Julia 122.07, 122.08,220.03Romani, Roger W. 410.09

Romanowsky, Aaron J. 222.07, 222.08Romanzin, Claire 205.04Rosanova, Alberto 123.57Rosenfeld, Katharine 322.22Ross, Ashley 410.07Ross, J. 419.06Ross, Nicholas P. 221.01Roth, Markus 123.54Rouillard, Alexis 212.05, 216.01Rouppe van der Voort, Luc 313.02Rowe, Jason 120.01, 120.06Royster, Marc 213.01Rozo, Eduardo 221.05Ruan, Guiping 303.03Rubio Da Costa, Fatima 409.06,414.04Ruel, Jonathan 405.07Rugheimer, Sarah 102.01Rupen, Michael P. 204.07Rusin, Vojtech 323.16Rust, Bert W. 121.21Rust, Thomas 414.06Ryan, Daniel 123.15, 123.37Ryan, James 415.01Ryan, Russell E. 417.06Ryde, Nils 418.04Ryer, Holly 320.12Rykoff, Eli S. 221.05Saar, Steven H. 123.43, 123.44,322.03, 322.08, 323.06Sadowski, Aleksander 204.01, 204.04Saglia, Roberto 213.06Saha, Abhijit 319.04Sahnow, David J. 122.07, 122.08Saigo, Kazuya 223.02Saint-Hilaire, Pascal 123.11, 123.31Saintonge, Amelie 222.01Sainz Dalda, Alberto 123.14Saito, Masao 223.02Sajina, Anna 206.08, 222.13, 222.16,222.17Salama, Farid 114.04, 119.06, 214.04Salome, Philippe 417.08Salvo, Chris 121.19, 121.20Samec, Ronald G. 219.09, 219.10,219.11, 420.03Sami, Mona 219.05Sana, Hugues 122.07, 122.08Sanchez, Richard L 320.08Sanders, David B. 206.07Saniga, Metod 323.16Sankrit, Ravi 412.04Sansone, Steve 415.02Sansonetti, Craig J 119.02Santos, Felipe A 206.04, 222.02,222.11Sarajedini, Ata 420.06Saral, Gozde 223.07Sardane, Gendith 423.02Sasselov, Dimitar D. 102.05, 120.23,219.15Sasselov, Dimitar 102.04Sauter, Patrick 419.03Savage, Maureen L. 418.03Savage, Sabrina 123.30, 312.06,323.20

Savani, Neel 212.05Savcheva, Antonia 303.01, 322.15,323.10, 323.37Savin, Daniel Wolf 119.05, 119.07,119.11, 323.53, 408.06Savolainen, Tuomas 221.15Saygac, Talat 223.07Scarlata, Claudia 417.06Schad, Thomas A. 123.58, 302.04Schaefer, Bradley E. 110.01, 306.04,412.02Schaeffer, Derek 305.01Schaible, Micah J 119.12Schanche, Nicole 323.47Schatz, Dennis L. 320.01Schechner, Sara 203.07Scherrer, Philip H. 218.42Schiavon, Ricardo P. 223.13Schiller, Quintin 107.02Schiller, Stephen J. 420.01Schlafly, Eddie 220.05Schlegel, David J. 410.07Schmelz, Joan T. 323.27Schmidt, Werner 119.06Schmit, Donald 323.09Schmitt, Henrique R. 404.05, 417.08Schneider, Donald P. 221.01Schneider, Nicola 223.01Schonfeld, Samuel J. 323.23Schou, Jesper 123.11Schrecengost, Zachariah 219.07Schrenk, Ryan 107.01Schrijver, Carolus J. 123.16, 321.02,323.19Schrijver, Karel 218.10, 218.14, 313.03Schroeder, James W 409.05Schuck, Peter W. 103.03Schuler, Simon C. 102.06Schuler, Timothy 323.20Schultz, Gregory R. 306.01Schulz, Norbert S. 421.01Schunker, Hannah 202.01Schwalm, D. 119.07Schwartz, Richard A. 111.01, 123.23,323.49Schwerin, Theresa 316.01Schwortz, Andria C. 320.08Sciamma-O'Brien, Ella 114.04, 214.04Scolnic, Daniel 412.07Scott, Roger B. 323.44Scowcroft, Victoria 421.03Scowen, Paul A. 215.05Scullion, Eamon 212.01Seader, Shawn 120.01, 120.03,120.04, 120.06Seager, Sara 200.01, 311.06Seaton, Daniel B 323.16, 422.03Segreto, Alberto 421.04Segura, Antigona 102.01Seibert, Mark 421.03Seitzer, Patrick 316.05Sen, Asoke K 122.18Serabyn, Gene 113.07, 311.07Shaklan, Stuart 311.06Shanks, Kimberly 120.17Share, Gerald H. 111.01, 123.03

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Sharykin, Ivan 104.03, 123.10,123.35Shaw, Michael S. 410.09Shaw, Richard A. 121.07, 121.09Shebs, Travis 219.11, 420.03Sheeley, Neil R. 203.02Shen, Chengcai 414.02Shen, Yue 221.01, 410.07Sherrill, M. 305.02Shi, Ji-Ming 419.08Shiao, Bernie 322.04Shih, Albert Y. 123.61, 123.62, 123.64,218.39Shih, Hsin-Yi 206.07Shimony, Assaf 413.01Shin, Seulki 123.42Shiota, Daikou 212.05Shipp, Stephanie 316.01Shkolnik, Evgenya 107.04Shoup, Jenae 219.08Shvarts, Dov 413.01Siana, Brian D. 417.06Sidery, Trevor 411.03Siegal-Gaskins, Jennifer M. 115.07Siegmund, Oswald 123.57Siemiginowska, Aneta 410.05Siemion, Andrew 204.07, 405.06Silva, Andrea Ludovina 222.13Silva, David R. 322.07Silverman, B. S 122.23Simet, Melanie 206.01Simpson, Janet P. 223.05Simunac, Kristin 323.65Singer, Leo 411.03Singh, Harinder P 219.07Singh, Sukhdeep 423.04Sinkovits, Robert 120.22Siverstein, Michele L 120.26Skidmore, Warren 122.18Skiff, Frederick 409.05Skogsrud, Haakon 313.02Slane, Patrick O. 412.05Slater, Stephanie 306.02, 320.02Slater, Timothy F. 306.02, 320.02,320.08Slatten, Kenneth J. 120.26Slavin, Jonathan David 220.16Sliski, David 102.03, 120.25Sloan, G. C 223.11Smith, David M. 123.02, 123.64Smith, Denise A. 306.01, 316.01,316.02, 316.03Smith, Graeme H. 404.07Smith, Howard Alan 206.07, 213.03,215.03, 215.07, 220.13, 223.01Smith, Jeffrey C 120.05, 120.08Smith, Jeffrey C. 120.04Smith, Matthew W 321.11Smith, Myron 322.04Smith, Nathan 121.16Smith, Paul S. 121.16, 221.19Smith, Randall K. 106.01, 121.22,122.14, 403.05, 405.02Snyder, Gregory F. 222.16Sobey, Alexander 123.61Soderberg, Alicia Margarita 421.08

Sohn, S. Tony 223.13Sohn, Young-Jong 223.08Sokol, Josh 418.01Song, Donguk 323.08Song, Hong-qiang 123.17Song, Inseok 419.09Song, Lei 413.04Sonnentrucker, Paul 114.01, 122.07,122.08Sonnentrucker, Paule 114.01, 122.07,122.08Soto, Emmaris 417.06Soto, Mario 319.01Soummer, Remi 301.05Souza, Steven P. 219.05Sparks, William B. 311.06Spekkens, Kristine 222.01Spencer, Jennifer L 218.41Spergel, David N. 101.01, 201.02Spiewak, Renée 121.12Spruck, K. 119.07St. Cyr, Orville Chris 218.04Staff, Jan E. 219.12Stairs, Ingrid H. 121.12Stancil, Phillip C. 413.04Stapelfeldt, Karl R. 113.08, 311.07Star, Kimberly Michelle 120.02Stark, Christopher C. 201.04Stark, Glenn 119.04Starr, Richard D. 123.23Stassun, Keivan 102.03, 102.06Steeghs, Danny 219.18Stein, Robert F. 103.02Steiner, James F. 219.17Steinitz, Gideon 211.02Stenborg, Guillermo A. 323.56Sterling, Alphonse C. 212.02, 408.03Stern, Daniel 221.12, 221.13Stork, Debra 320.02Stovall, Kevin 121.12Strachan, Leonard 323.50Strader, Jay 221.02, 222.08, 223.12,404.07Straus, Thomas 323.05Strauss, Michael A. 221.01Streblyanska, Alina 221.01Struminsky, Alexei 123.35Stubbs, Christopher 122.17, 319.04,405.01, 405.07Stuetzel, Julia 119.05Sturrock, Peter A. 211.02Stys, Jeffrey E. 218.44Su, Meng 213.04Su, Yingna 123.29, 218.20, 218.22,303.01, 323.52Sul, Cesar 120.17Sullivan, Peter 113.01, 113.03Sullivan, Shane 218.32Sumandal, Julienne 121.19, 121.20Sumi, Takahiro 210.05Sumi, Takahiro 319.03Summers, Frank 320.12Sun, Brian M 404.05Sun, Ming 417.08Sun, Xudong 103.06, 123.48, 323.64Sun, Xudong 103.06, 123.48, 323.64

Sunada, Eric 311.07Sundkvist, David 323.67Sung, Kwang Hyun 220.17Suzuki, Daisuke 210.04Swain, Mark R. 122.09Swift, Carrie 219.02Swift, Jonathan 314.04Szabados, Laszlo 219.06Szabo, Robert 219.06Szkody, Paula 322.07, 412.01Tachihara, Kengo 223.02Takahashi, Satoko 223.02Takamiya, Marianne Y. 318.10Tamura, Motohide 301.03Tamura, Naoyuki 223.13Tang, Sumin 410.05Tarbell, Theodore D. 123.63, 203.03Tarr, Lucas 422.04Tatge, Coty 320.08Tayal, Swaraj S. 119.01Taylor, Gregory 422.06Taylor, Isabel 421.02Taylor, Joanna M. 122.07, 122.08Tchekhovskoy, Alexander 204.01Tegler, Stephen C. 214.03Tegmark, Max 304.04Tembe, Mita 323.14Temi, Pasquale 417.08Tenenbaum, Peter 120.01, 120.03,120.06Tenneti, Ananth 115.02Teplitz, Harry I. 417.06Test, John H 415.01Testa, Paola 313.05, 323.22Thanjavur, Karun 405.01Theissen, Christopher 322.10Thomas, Jens 213.06Thomas, Ryan 405.01Thomas, Sandrine 223.03Thompson, Barbara J. 218.38Thompson, Michael 123.54Thompson, Randy 322.04Thompson, Susan E. 113.04Thompson, William T. 123.57Thomson, Mark 311.06Tian, Hui 313.06, 323.10Tian, QiGuo 417.05Timmons, Ryan 313.01Timokhin, Andrey 121.10, 121.11Tipler, Frank 304.01Tisserand, Patrick 322.17Title, Alan M. 123.16, 123.19Titov, Viacheslav 111.04, 212.04,218.08, 312.02Tiwari, Sanjiv Kumar 409.04Tobin, John J. 220.12Tohline, Joel E. 219.12Tolbert, Anne K 111.01, 123.23, 323.49Tomczyk, Steven 323.24Tonry, John L. 122.17Toomey, James Edward 417.01Toomre, Juri 211.04Torok, Tibor 212.04, 218.08, 312.02Torres, Guillermo 322.01Torres, Manuel 219.18Trantham, Matt 413.01

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Traub, Wesley A. 311.04, 311.07Trauger, John T. 311.07Triaud, Amaury H. M. J. 416.02Tripathi, Shreekrishna 403.01Tripathy, Sushanta 218.21Tritschler, Alexandra 112.02, 323.04Troeltzsch, John 122.11Troja, Eleonora 421.04Troland, Thomas H. 419.01Trouille, Laura 410.01Trungg, Dinh-V 417.08Tseng, Shui-Ay 322.04Tumlinson, Jason 220.03Tunbridge, Ben 120.21, 411.01Turmon, Michael 123.52Turnbull, Margaret C. 311.06Turner, David G. 110.03, 318.09Turnshek, David 423.02Tweed, Benjamin 220.02Twicken, Joseph D. 120.01, 120.06Twiggs, Bob James , 122.23Tylka, Allan J. 111.01Tzeferacos, Petros 412.03Tzioumis, A. 204.05Ubeda, Leonardo 319.06Udalski, Andrzej 319.03Ugarte-Urra, Ignacio 312.05Unwin, Stephen C. 201.01, 311.07Upton, Kathleen 214.04Upton, Lisa 103.01D, 218.09Urbain, Xavier 119.05Urban, Alex 411.03Uritsky, Vadim 111.06Urry, C. Megan 410.03, 410.08Vacca, William D. 418.04Vaccari, Mattia 206.08Valsecchi, Francesca 102.08Van Ballegooijen, Adriaan A. 123.29,218.20, 321.02van Belle, Gerard 404.05van der Avoird, Ad 413.04Van Der Bliek, Nicole S. 122.20,223.03Van Der Holst, Bart 323.42Van Gorkom, Jacqueline H. 116.01Van Hamme, Walter V. 219.09, 219.10van Kempen, Tim 223.02Van Weeren, Reinout J. 206.04, 222.03Vanderburg, Andrew 120.12, 121.17Vanderlinde, Keith 405.01Vanderspek, Roland Kraft 113.02,113.03VanderWiel, Scott 204.07VanHilst, Michael 320.06Vargas Domínguez, Santiago 123.45Varlotta, Angelo 219.22Vaulin, Ruslan 318.13, 411.06Vazquez, Billy 221.17Vecchio, Alberto 411.03Vecchio, Antonio 323.04Vedovato, Gabriele 411.04Veitch, John 411.03Venkataramanasastry, Aparna 414.03Verschuur, Gerrit L. 115.04Viall, Nicholeen 323.15, 402.02Vican, Laura 419.07, 419.09

Vidali, Gianfranco 119.09, 205.03Viel, Matteo 221.01Vikhlinin, Alexey 222.03Villasenor, Jesus Noel 321.11Vitale, Salvatore 411.03, 411.04Vivas, Katherina 319.01Vo, Richard 222.08Vogel, Julia 123.64Vogeley, Michael S. 221.06, 222.09,318.08Voulgaris, Aristeidis 323.16Vourlidas, Angelos 212.05, 212.06,323.28, 323.58, 402.02Voyer, Elysse 417.06Vrtilek, Jan M. 417.08Vrtilek, Saeqa Dil 405.05Walker, Constance E. 316.05Walker, Kyle M. 413.04Wallace, Colin Scott 320.07Walters, Angela 107.01Walton, Dom 221.12Wan, Wesley 413.01Wang, Amanda 422.08Wang, Haimin 111.04, 123.04,123.32, 414.01Wang, Tongjiang 323.30, 323.48,323.54, 408.05Wang, Yi-Ming 323.66Wang, Yiran 423.03Wang, Yuming 111.04Wang, Zhitao 323.45Wang, Zhong 213.03Wardle, John F. C. 204.06, 219.23,219.24Wardle, M. 213.01Warfield, Keith 311.07Wargelin, Bradford J. 321.03Warren, Harry P 111.05Warren, Harry 123.01, 123.07, 312.05Warren, Steven R. 215.04Watson, Fraser 112.02Watson, William 102.07Wawro, Martha 320.11Webb, David F. 218.04Webb, David 311.06Webber, Matthew 102.02Weber, Maria A. 211.01DWeber, Mark A. 313.06, 323.17Weber, Thomas 409.03Wegner, Gary A. 206.02, 213.06Weil, Kathryn 221.16Weinberg, David H. 221.01Weiner, Neal 115.08Weintroub, Jonathan 414.05Weisenburger, Kolby L. 102.09Welch, Douglas L. 110.02, 322.17Welsch, Brian 103.05, 123.49Werthimer, Dan 405.06West, Andrew A. 102.09, 320.04,322.10, 322.12, 322.14, 322.15,404.04West, Ed 323.11West, Matthew J 422.03Westerhoff, Thomas 122.21Weyant, Anja 121.15Wheatland, Michael S 323.19

White, Martin 221.01White, Richard L. 322.04White, Russel J. 120.19White, Stephen M. 111.01, 123.60,123.64, 323.23, 323.45White, Travis 107.01Whitney, Barbara 223.05Wiemer, Doug 122.11Wiktorowicz, Sloane 219.21Wilkes, Belinda J. 410.06Williams, Brian J. 412.04Williams, G. Grant 121.16Willingale, Richard 122.14, 405.02Willis, Sarah 215.03Willmar, Christopher 410.06Willner, Steven P. 213.03, 319.07Wilms, Jörn 122.14, 403.05, 405.02Wilner, David J. 223.06, 322.21, 322.22Wilson, B. G 305.02Wilson, Colleen 123.62Wilson, Robert W. 415.02Windhorst, Rogier A. 417.06Winebarger, Amy R. 312.03, 312.06,323.11, 323.20, 323.41, 409.04Wing, Joshua 206.05Winkler, P. Frank 412.04Winn, Joshua N. 113.01, 113.02,113.03Winske, Dan 305.01Winter, Henry D. 121.22, 323.14Winters, Jennifer G. 120.26Witzel, Gunther 213.03Wolf, A. 119.07Wolfire, Mark G. 215.04Wolk, Scott J. 220.12, 419.04Wood, Jeremy R 321.07Wood-Vasey, W. Michael 121.15,221.01Woods, Thomas N. 123.07Woolsey, Lauren N. 402.05Woytko, Gregory 123.57Wray, Alan A 103.04Wright, Jason 223.10, 322.03Wright, Paul J. 123.43Wu, S. T. 323.31Wuelser, Jean-Pierre 123.20Wyper, Peter 323.46Wysocki, Daniel 219.07Xie, Hong 218.04Xie, Yanxia 119.10Xu, Yan 123.04, 414.01Xu, Zhi 414.01Yamada, Masaaki 323.70, 403.02Yamada, Yoshihiko 223.13Yamaguchi, Hiroya 403.05Yan, Lin 222.16Yang, Benhui H 413.04Yang, Heesu 323.08Yang, Seungwon 220.17Yaqoob, Tahir 410.08Yashiro, Seiji 303.06Yeates, Anthony R 211.03Yeche, Christophe 221.01, 410.07Yee, Jennifer C 311.02Yermakova, Anya 415.02Yoo, Jongsoo 323.70, 403.02

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Yoon, Seokjun 421.02Yoon, Seokkwan S 323.02Yoon, Suk-Jin 223.13York, Don 221.01Young, Aleida 402.03Young, C. Alex 218.38, 218.47Young, Michael 319.01, 319.02Young, Peter R. 106.03, 302.02,323.33, 323.66Young, Rachel P. 419.06Yurchyshyn, Vasyl B. 218.11, 323.01Yusef-Zadeh, Farhad 213.01Zack, Kevin 122.23Zakamska, Nadia L. 400.01Zank, Gary 323.62

Zatsarinny, Oleg 119.01Zauderer, B. Ashley 421.08Zehavi, Idit 221.01Zeiler, Michael 323.16Zeng, Lingzhen 415.02Zeng, Zhicheng 123.04, 123.09Zezas, Andreas 215.07, 223.12,319.05Zhang, Jie 123.17, 218.06, 218.28,323.55Zhang, Qizhou 215.02, 404.08Zhang, Tianxi 204.03, 304.03Zhao, Jingkun 219.16Zhao, Junwei 103.06, 202.02, 202.03,218.05

Zhao, Xuepu 323.60Zheng, Haoxuan 318.07Zheng, Zheng 221.05Zhou, HongYan 417.05Zhu, Emily 421.02Zhu, Ling 319.03Zhu, Qirong 215.08Zimovets, Ivan 104.03, 123.35Zingale, Michael 121.01Zonca, Andrea 120.22Zuccarello, Francesca 123.39Zuckerman, Ben M. 419.09Zurbuchen, Thomas H. 402.03

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224th aas - american astronomical society · 224th aas boston, ma – june, 2014 meeting abstracts...

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